On Generalised Statistical Equilibrium and Discrete Quantum Gravity (Springer Theses) 3030909689, 9783030909680

Citation preview

Springer Theses Recognizing Outstanding Ph.D. Research

Isha Kotecha

On Generalised Statistical Equilibrium and Discrete Quantum Gravity

Springer Theses Recognizing Outstanding Ph.D. Research

Aims and Scope The series “Springer Theses” brings together a selection of the very best Ph.D. theses from around the world and across the physical sciences. Nominated and endorsed by two recognized specialists, each published volume has been selected for its scientific excellence and the high impact of its contents for the pertinent field of research. For greater accessibility to non-specialists, the published versions include an extended introduction, as well as a foreword by the student’s supervisor explaining the special relevance of the work for the field. As a whole, the series will provide a valuable resource both for newcomers to the research fields described, and for other scientists seeking detailed background information on special questions. Finally, it provides an accredited documentation of the valuable contributions made by today’s younger generation of scientists.

Theses may be nominated for publication in this series by heads of department at internationally leading universities or institutes and should fulfill all of the following criteria • They must be written in good English. • The topic should fall within the confines of Chemistry, Physics, Earth Sciences, Engineering and related interdisciplinary fields such as Materials, Nanoscience, Chemical Engineering, Complex Systems and Biophysics. • The work reported in the thesis must represent a significant scientific advance. • If the thesis includes previously published material, permission to reproduce this must be gained from the respective copyright holder (a maximum 30% of the thesis should be a verbatim reproduction from the author’s previous publications). • They must have been examined and passed during the 12 months prior to nomination. • Each thesis should include a foreword by the supervisor outlining the significance of its content. • The theses should have a clearly defined structure including an introduction accessible to new PhD students and scientists not expert in the relevant field. Indexed by zbMATH.

More information about this series at https://link.springer.com/bookseries/8790

Isha Kotecha

On Generalised Statistical Equilibrium and Discrete Quantum Gravity Doctoral Thesis accepted by Humboldt-Universität zu Berlin, Berlin, Germany

Author Dr. Isha Kotecha Qubits and Spacetime Unit Okinawa Institute of Science and Technology Okinawa, Japan

Supervisor Dr. Daniele Oriti Arnold Sommerfeld Center for Theoretical Physics Ludwig-Maximilians-Universität München Munich, Germany

ISSN 2190-5053 ISSN 2190-5061 (electronic) Springer Theses ISBN 978-3-030-90968-0 ISBN 978-3-030-90969-7 (eBook) https://doi.org/10.1007/978-3-030-90969-7 © The Editor(s) (if applicable) and The Author(s), under exclusive license to Springer Nature Switzerland AG 2022 This work is subject to copyright. All rights are solely and exclusively licensed by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, expressed or implied, with respect to the material contained herein or for any errors or omissions that may have been made. The publisher remains neutral with regard to jurisdictional claims in published maps and institutional affiliations. This Springer imprint is published by the registered company Springer Nature Switzerland AG The registered company address is: Gewerbestrasse 11, 6330 Cham, Switzerland

Where the voice of the wind calls our wandering feet, Through echoing forest and echoing street, With lutes in our hands ever-singing we roam, All men are our kindred, the world is our home. —Sarojini Naidu, in Wandering Singers

For my grandparents, my guiding stars and my parents, my guiding lights

Supervisor’s Foreword

It is a pleasure to introduce to you this work by Dr. Kotecha, resulting from her Ph.D. thesis at the Max Planck Institute for Gravitational Physics in Potsdam, Germany. It is a top-quality presentation of a difficult and fascinating area of research, dealing with truly foundational topics in theoretical physics, combining technical as well as conceptual challenges. It includes the details of the original research carried out by the author and a lucid and insightful discussion of the context and implications of this research, providing a useful introduction to the field. The general topic of this work is the definition of a fully covariant quantum statistical mechanics framework for quantum gravity degrees of freedom. The problem of defining statistical mechanics in a background independent context when the gravitational field and geometry are themselves dynamical is an open issue in theoretical physics and notoriously challenging at both conceptual and technical levels. When the gravitational field and spacetime are themselves quantized, the challenge is way bigger. Further, in the context of quantum gravity approaches where spacetime and the gravitational field (classical or quantum) do not feature among the basic entities but have to be reconstructed from the collective behaviour of different, more fundamental quantum degrees of freedom, the challenge is even greater. Yet, this was the challenge that Dr. Kotecha set for herself and the context of her Ph.D. thesis. The motivation for tackling this challenge is as big as its difficulties. A proper understanding of the interplay between gravitational, quantum, and thermal effects is of paramount importance, in fact, well beyond its foundational significance and the formal definition of a theory of quantum gravity. It is also necessary, for example, for understanding the physics of quantum black holes and cosmological horizons, even in a semi-classical regime, and for tackling several issues concerning the physics of the primordial universe. The specific formal context of the thesis is that of discrete quantum gravity and of tensorial group field theory models, but the research questions tackled by Dr. Kotecha, the technical strategies adopted to answer them, and the potential impact of her results go way beyond this specific context. On the one hand, the tensorial group field theory formalism has been chosen since, due to its technical peculiarities, it allows for the rigorous implementation of conceptual and mathematical strategies toward a ix

x

Supervisor’s Foreword

definition of quantum statistical mechanics, which have been proposed for quantum gravity more generally. On the other hand, other quantum gravity formalisms like spin foam models and loop quantum gravity are very closely related to tensorial group field theories and share the same type of discrete fundamental degrees of freedom. All this is eloquently explained in the review part of this work, which clarifies conceptual issues, previous research on this topic, and the required technical background. The original research at the basis of the present book is the result of four main research projects. The first two tackled the issue of defining statistical equilibrium in full quantum gravity. This is an absolutely non-trivial problem since fundamental quantum gravity lacks any preferred notion of time, which is usually needed to define what equilibrium means. The first project provided a few candidate constructions of equilibrium states in group field theory: one based on KMS conditions and rooted in the algebraic definition of the theory (in the spirit of the so-called ‘thermal time hypothesis’) and associated to various internal symmetries of the corresponding algebra of observables, interpreted as possible ‘temporal’ evolution flows associated to internal degrees of freedom of the models used as ‘relational clocks’; another resting on the deparametrization of the same theory, with any such relational clock acquiring the standard role as external evolution parameter, in some approximation; and yet another one based on Jaynes’ entropy maximization principle at fixed average volume. The second project expands and generalizes this last approach, and it defines statistical equilibrium based on Jaynes’ entropy maximization principle, subject to general macroscopic constraints, providing then a number of concrete examples. The procedure was applied to systems of classical and quantum tetrahedra, the degrees of freedom shared by discrete quantum gravity, spin foam models, and group field theories. In fact, it can also be seen as a fundamental definition of the group field theory formalism, as a background independent statistical mechanics system of quantum simplices. This second work also rests on a geometric formulation of statistical mechanics applied to quantum gravity, which is of great interest in itself. The last two projects concerned the construction of a thermofield dynamical framework for group field theories, and associated thermal representations, and studied coherent states associated to such thermal representations. Next, they combined the thermofield formalism and the associated coherent states to study the emergent cosmological dynamics from group field theories and the role of thermal fluctuations in it. The equilibrium states for quantum gravity systems that had been developed in the previous projects found then a first physical application. The whole construction is highly non-trivial at the mathematical level, and it is a solid basis for a number of current and future physical applications. But the book is far from a simple collection of research results. It is a coherent and organic exposition of this foundational research area, starting from the conceptual motivations, developing the mathematical foundations, and then presenting in a logically crystal-clear manner the various developments. The author provides us with a very clear vision of the field and presents it in an insightful and deep manner. Moreover, it is, quite simply, a pleasure to read: the ideas are clearly exposed and logically connected to one another, the more formal aspects presented with rigour but no unnecessary or pedantic detail, the physical aspects duly emphasized and well

Supervisor’s Foreword

xi

placed in a broader context, and the whole presentation is full of interesting insights. I am certain that the reader will enjoy it as much as I did. Munich, Germany March 2021

Dr. Daniele Oriti Senior researcher and group leader, Heisenberg Grant—DFG

Abstract

Statistical equilibrium configurations are known to be important in the physics of macroscopic systems with a large number of constituent degrees of freedom. They are expected to be crucial also in discrete quantum gravity, where dynamical spacetime should emerge from the collective physics of the underlying quantum gravitational degrees of freedom. However, defining statistical equilibrium in a background independent system is a challenging open issue, primarily due to the absence of absolute notions of time and energy. This is especially so in non-perturbative quantum gravity frameworks that are devoid of usual space and time structures. In this thesis, we investigate aspects of a generalisation of statistical equilibrium, specifically of the Gibbs states, suitable for background independent systems. We emphasise on an information theoretic characterisation for equilibrium based on the maximum entropy principle. Subsequently, we explore the resultant generalised Gibbs states in a discrete quantum gravitational system, composed of many candidate quanta of geometry of combinatorial and algebraic type (or, convex polyhedra). We utilise their field theoretic formulation of group field theory and various many-body techniques for our investigations. We construct concrete examples of quantum gravitational generalised Gibbs states, associated with different generators, e.g. geometric volume operator, momentum operators and classical closure constraint for polyhedra. We further develop inequivalent thermal representations based on entangled, two-mode squeezed, thermofield double vacua, which are induced by a class of the generalised Gibbs states. In these thermal representations, we define a class of thermal condensates which encode statistical fluctuations in volume of the quantum geometry. We apply these states in the condensate cosmology programme of group field theory, where the key idea is that a macroscopic homogeneous spacetime can be approximated by a dynamical condensate phase of the underlying quantum gravity system. We study the relational effective cosmological dynamics extracted from a class of free group field theory models, for homogeneous and isotropic spacetimes. We find the correct classical limit of Friedmann equations at late times, with a bounce and accelerated expansion at early times.

xiii

Acknowledgements

Science is a journey driven by curiosity and learning. For me, this journey which began many years ago in high school has reached a personal milestone with the completion of this thesis and my Ph.D. It would have been impossible without the help, encouragement and friendship of many people, to whom I am deeply grateful. It is fortunate, as a young researcher, to be able to immerse in as stimulating an environment as that of the Albert Einstein Institute and the Humboldt University of Berlin. I am indebted to Daniele Oriti, Hermann Nicolai, Deutscher Akademischer Austauschdienst (DAAD) and International Max Planck Research School for making this possible. I am especially thankful to Daniele for his mentorship and constant guidance, which helped me greatly to navigate through research topics and workings in academia. In addition to patiently guiding me through the dense literature for tackling these questions, he introduced me to important foundational problems in the field, while also encouraging me to explore topics of personal interest. I am grateful to Philipp Höhn and the Okinawa Institute of Science and Technology for support during the process of publication of this thesis here in the Springer Theses book series. My Ph.D. experience was enriched by the support of several people. Many special thanks are due to my collaborators, Goffredo Chirco and Mehdi Assanioussi, for numerous insightful discussions and friendly advice. I am also sincerely grateful to Rob Myers and Sylvain Carrozza, for the wonderful opportunity to spend some time at the Perimeter Institute as a visiting graduate fellow. I am thankful to Joseph Ben Geloun, Axel Kleinschmidt, Sandra Faber, Sumati Surya and Amihay Hanany for their help, at various different stages during and before the start of my Ph.D. My time at AEI was made enjoyable by the presence of many friends and colleagues. For this, I would like to thank Alexander Kegeles, Claudio Paganini, Johannes Thürigen, Seungjin Lee, Mingyi Zhang, Ana Alonso-Serrano, Olof Ahlén, Alice Di Tucci, Caroline Jonas, Sebastian Bramberger, Lars Kreutzer, Jan Gerken and Hugo Camargo. I am particularly thankful to Alexander for a thorough reading of an earlier version of this thesis and valuable comments, and to Claudio for help with the German translation of the summary. Working at AEI, living in Germany and completing the Ph.D. was made a lot easier due to the proactive support of xv

xvi

Acknowledgements

several people, to whom I am very grateful: Anika Rast, Darya Niakhaichyk and Constance Münchow at AEI; Bettina Wandel at DAAD; Jennifer Sabernak and Carolin Schneider at Potsdam International Community Center; and, Daniel Schaan and Milena Bauer at HU-Berlin. To my loving family, I am forever grateful. To my parents, Kotecha and Patel, for their open-mindedness and inspiration. To Kishan, Priyanka and Riddhi, for being my pillars of strength. Foremost, to my husband Meet, for his relentless support, unwavering faith and for being a true friend, ever since this journey began.

Contents

1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1.1 Thermal Physics, Gravity and Quantum Theory . . . . . . . . . . . . . . . . . 1.2 Why Search for Quantum Gravity . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1.3 Outline of the Thesis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . References . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

1 1 5 6 10

2 Generalised Statistical Equilibrium . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.1 Rethinking Time in Mechanics . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.1.1 Preliminaries: Presymplectic Mechanics . . . . . . . . . . . . . . . . . 2.1.2 Deparametrization . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.2 Generalised Gibbs Equilibrium . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.2.1 Characterising Gibbs States . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.2.2 Past Proposals . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.2.3 Thermodynamical Characterisation . . . . . . . . . . . . . . . . . . . . . 2.2.4 Modular Flows and Stationarity . . . . . . . . . . . . . . . . . . . . . . . . 2.2.5 Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.3 Generalised Thermodynamics . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.3.1 Thermodynamic Potentials and Multivariable Temperature . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.3.2 Single Common Temperature . . . . . . . . . . . . . . . . . . . . . . . . . . 2.3.3 Generalised Zeroth and First Laws . . . . . . . . . . . . . . . . . . . . . . Appendix: Stationarity with Respect to Constituent Generators . . . . . . . . References . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

15 17 17 21 22 23 28 30 32 34 36

3 Many-Body Quantum Spacetime . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3.1 Atoms of Quantum Space and Kinematics . . . . . . . . . . . . . . . . . . . . . 3.2 Interacting Quantum Spacetime and Dynamics . . . . . . . . . . . . . . . . . 3.3 Generalised Equilibrium States . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3.4 Effective Statistical Group Field Theory . . . . . . . . . . . . . . . . . . . . . . . References . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

45 46 51 53 54 58

36 38 39 40 42

xvii

xviii

Contents

4 Group Field Theory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.1 Bosonic Group Field Theory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.1.1 Degenerate Vacuum and Fock Representation . . . . . . . . . . . . 4.1.2 Useful Bases . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.1.3 Weyl Algebra . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.1.4 Translation Automorphisms . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.2 Deparametrization in Group Field Theory . . . . . . . . . . . . . . . . . . . . . . 4.2.1 Classical System . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.2.2 Quantum System . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Appendix 1: *-Automorphisms for Translations . . . . . . . . . . . . . . . . . . . . Appendix 2: Strong Continuity of Unitary Translation Group . . . . . . . . References . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

61 64 64 66 69 71 74 74 81 86 88 91

5 Thermal Group Field Theory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.1 Generalised Gibbs States . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.1.1 Positive Extensive Operators . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.1.2 Momentum Operators . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.1.3 Constraint Functions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.2 Thermofield Doubles, Thermal Representations and Condensates . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.2.1 Preliminaries: Thermofield Dynamics . . . . . . . . . . . . . . . . . . . 5.2.2 Degenerate Vacuum and Zero Temperature Phase . . . . . . . . . 5.2.3 Thermal Squeezed Vacuum and Finite Temperature Phase . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.2.4 Coherent Thermal Condensates . . . . . . . . . . . . . . . . . . . . . . . . 5.3 Thermal Condensate Cosmology . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5.3.1 Condensates with Volume Fluctuations . . . . . . . . . . . . . . . . . . 5.3.2 Effective Group Field Theory Dynamics . . . . . . . . . . . . . . . . . 5.3.3 Smearing Functions and Reference Clocks . . . . . . . . . . . . . . . 5.3.4 Relational Functional Dynamics . . . . . . . . . . . . . . . . . . . . . . . . 5.3.5 Effective Cosmology with Volume Fluctuations . . . . . . . . . . 5.3.6 Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . Appendix 1: Gibbs States for Positive Extensive Generators . . . . . . . . . . Appendix 2: KMS Condition and Gibbs States . . . . . . . . . . . . . . . . . . . . . Appendix 3: Strong Continuity of Map U X . . . . . . . . . . . . . . . . . . . . . . . . Appendix 4: Normalisation of Gibbs State for Closure Condition . . . . . References . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

95 97 98 105 111

6 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.1 Towards Generalised Equilibrium Statistical Mechanics . . . . . . . . . . 6.2 Towards Thermal Quantum Spacetime . . . . . . . . . . . . . . . . . . . . . . . . . 6.2.1 Many-Body Formulation and Group Field Theory . . . . . . . . 6.2.2 Generalised Gibbs States . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.2.3 Thermofield Double Vacua and Inequivalent Representations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.2.4 Condensate Cosmology with Volume Fluctuations . . . . . . . .

123 124 128 130 132 135 136 137 139 141 144 152 153 157 160 161 162 167 167 169 169 170 172 173

Contents

xix

6.3 Final Remarks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 175 References . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 176

Chapter 1

Introduction

To doubt everything or to believe everything are two equally convenient solutions; both dispense with the necessity of reflection. —Henri Poincaré

1.1 Thermal Physics, Gravity and Quantum Theory There are three foundational pillars of physics, namely thermal physics,1 gravity and quantum theory. Any fundamental theory of nature must be built atop them. A deep interplay between the three was unveiled by the discovery of black hole entropy [2–4] and radiation [5]. As a direct consequence, a multitude of new conceptual insights arose, along with many puzzling questions that continue to be investigated still after decades. In particular, a black hole is assigned physical entropy, S=

A 42P

(1.1)

 scaling linearly with the area A of its horizon (to leading order), where  P = G/c3 is the Planck length [2, 3, 6–8]. This led to several distinct lines of thoughts, in turn leading to various lines of investigations, like holography [9, 10] and thermodynamics of gravity [11, 12]. Further, early attempts at understanding the physical origin of this entropy made the relevance of quantum entanglement evident [13, 14], thus contributing significantly to the current prolific interest in connections between gravitational physics and quantum information theory [15–22]. 1

By thermal physics, we mean statistical physics, thermodynamics, and many-body theory in general. For some discussions on the significance of many-body physics in the context of quantum gravity, see for instance [1].

© The Author(s), under exclusive license to Springer Nature Switzerland AG 2022 I. Kotecha, On Generalised Statistical Equilibrium and Discrete Quantum Gravity, Springer Theses, https://doi.org/10.1007/978-3-030-90969-7_1

1

2

1 Introduction

In fact, Bekenstein’s original arguments [3] were also information-theoretic in nature, utilising insights from Jaynes’ realisation [23, 24] of equilibrium statistical mechanics based on maximising information entropy under a given set of macrostate constraints.2 Black hole entropy was understood as information entropy [3], quantifying our lack of knowledge about the specifics of the system, here of the detailed configuration of the black hole with respect to an exterior observer. For instance, a stationary black hole is classically characterised completely by its mass M, charge Q and angular momentum J . An outside observer could in principle measure the macrostate of this peculiar thermodynamic system in terms of this set of observables, without detailed knowledge of its quantum gravitational microstate. They could write down its entropy as the Shannon or von Neumann entropy [3], S = − ln ρρ

(1.2)

in a statistical state ρ such that {Mρ = M, Qρ = Q, J ρ = J }, where M, Q and J are observables defined on some suitable underlying state space of the system, and . denotes a statistical average. Then, entropy S measures the uncertainty of the system being in a particular quantum microstate compatible with the given thermodynamic macrostate. We will return to a detailed discussion of these, and other related aspects of Jaynes’ method in Sect. 2.2, particularly in the context of background independent systems. For now, let us mention two important features encountered here, which as we shall see later, are intrinsic also to the generalised equilibrium statistical mechanical framework developed as part of this thesis. Firstly, black hole entropy can be understood as a measure of the lack of knowledge of a given observer about the system, or a measure of inaccessibility of information [3, 13, 27, 28]; and, this inaccessibility of (correlated3 ) information, here due to the presence of a horizon, is the reason for its thermality. Secondly, the notion of information and statistical states used here is subjective, in the sense that it refers to the state of knowledge of the given observer [3, 23]. Thus, the associated notion of thermality is inherently observer-dependent. This brings us to a discussion of some fundamental and universal features related to thermality in gravitational and quantum settings in general, which we think are valuable also to bear in mind while investigating candidate quantum gravitational systems. The intriguing connections between thermality, gravity and quantum theory can be succinctly displayed in the following equation for the temperature associated with causal horizons,

2

As we will see in Sect. 2.2, these same insights are instrumental in our characterisation of statistical equilibrium in a background independent context [25, 26]. 3 Correlations between the relevant degrees of freedom across an information barrier is critical for having thermality, as we will discuss more below. These correlations could arise due to interactions, say in classical statistical systems coupled to a heat bath, or even purely from entanglement between two quantum statistical systems without any interactions. In fact, in Sect. 5.2 we will construct a family of thermal vacua, induced by a family of generalised Gibbs states, with entanglement between the underlying quantum gravitational degrees of freedom.

1.1 Thermal Physics, Gravity and Quantum Theory

T =

a  2π k B c

3

(1.3)

where a is the acceleration characterising the horizon, and k B is the Boltzmann’s constant. In the context of black holes, this is the well-known Bekenstein-Hawking temperature with a being the surface gravity, while in the setting of Rindler decomposition of Minkowski spacetime, it is the Unruh temperature. This is a remarkable formula, hinting at several important points. Notice that T is independent of the precise details of any matter degrees of freedom. Even though standard derivations of this equation utilise some quantum matter field along with a chosen dynamical model, the final expression is evidently independent of them. This suggests that T could be an inherent property of dynamical spacetime, and even more so because, besides the fundamental constants, it is completely characterised by the gravitational acceleration parameter a. In other words, this expression suggests that spacetime is hot, and any other matter field, if present, will then naturally equilibrate with it to acquire the same temperature [29]. This further suggests the existence of quantum microscopic degrees of freedom underlying a spacetime. Also, this temperature is intrinsically observer-dependent, due to the observer dependence of a. For instance, different Rindler observers with different accelerations will detect thermal radiation at different temperatures, according to the formula (1.3). In fact, spacetime thermodynamics is observer-dependent in general [29–31]. A vital feature that is not totally explicit in Eq. (1.3) is the fact that spacetime thermality is tightly linked to causal horizons, or null surfaces. In other words, it is tightly linked to the existence of information barriers, i.e. boundaries beyond which lies information that is inaccessible to a set of observers on the other side. In an algebraic setup for instance, this would be related to a pair of commuting algebras of observables associated with Kubo-Martin-Schwinger (KMS) states [32–34]. More generally, we notice that thermality originates from having inaccessible or hidden information that is correlated with information in a region that is accessed by an observer. In the special case of spacetime thermality then, the region of this hidden information is naturally demarcated by a horizon, which in turn is determined fully by the causal structure. Specifically for the class of equilibrium KMS states, equivalently Gibbs states for finite number of degrees of freedom, this thermality is linked further to periodicity in the two-point correlation functions of the algebra of observables [32–37]. This connection between quantum correlations, information barriers and thermality can be illustrated with a simple, yet important and widely utilised example of a thermofield double state [38, 39]. Consider the case of two bosonic, non-interacting oscillators, each described in the standard way by its own set of ladder operators, cyclic vacua, Fock Hilbert spaces and free (kinetic energy) Hamiltonians. The composite system is then given by ladder operators {aˆ 1 , aˆ 1† , aˆ 2 , aˆ 2† } satisfying the following commutation algebra, [aˆ i , aˆ †j ] = δi j , [aˆ i , aˆ j ] = [aˆ i† , aˆ †j ] = 0, for i, j = 1, 2. Notice that the algebras of the two oscillators, generated by these ladder operators, commute with each other. The individual vacua, given by aˆ i |0i  = 0, specify a vacuum | = |01  ⊗ |02  of the composite system, which in turn generates the full

4

1 Introduction

Hilbert space of a tensor product form. Then, a thermofield double, is a vector state of the full system, defined by  β   β = 1 e− 2 En |n1 ⊗ |n2 Zβ n

(1.4)

√ where |ni = (ai† )n |0i  / n! are the energy eigenstates of the individual oscillators with spectrum E n [38, 39]. This is an entangled state, with (maximum4 ) quantum correlations between the two oscillators. Then, the connection between the three aspects that we noted above can be demonstrated most directly by the fact that neglecting the degrees of freedom of either one of the oscillators (via partial tracing of the thermofield double) results in a (maximally entropic) thermal Gibbs state at inverse temperature β. In other words, any observer restricted5 to either one of these oscillators (in general, subsystems) will measure properties that are compatible with being in a thermal state, via observable averages of the associated restricted algebra;   and, this is a direct consequence of the full system being in an entangled state β , unlike the separable vacuum |. Such entangled states naturally also occur in systems with many degrees of freedom, including quantum field theories on flat and curved spacetimes. Prime examples are the relativistic Minkowski vacuum for uniformly accelerated observers, and the Hartle-Hawking vacuum for stationary observers outside a black hole [40–44]. Along the same lines, in the context of holographic theories, thermofield doubles of boundary conformal field theories are dual to bulk eternal AdS black holes [45]. In the context of discrete quantum gravity, we have constructed thermofield double vacua associated with a class of generalised Gibbs states [46], as will be discussed later in Sect. 5.2. We thus see that the notions of thermality, observer-dependence, quantum correlations, and accessibility of information (in turn related to causality when working with spacetime manifolds), all of which we will also encounter in this thesis, become deeply intertwined at the interface of quantum theory, gravity and thermal physics. It is at this interface, we believe, that further key insights into the nature of gravity await our discovery. Particularly with regards to the topic of this thesis, the formulation and investigation of thermal aspects of candidate quantum gravity frameworks may be vital to gain a more fundamental and detailed understanding of physical systems, like quantum black holes and early cosmological universe that are used often as theoretical laboratories for foundational research. For example, what ‘hot’ even means at Planck scales, where notions of energy and spacetime may be notably different or even absent, needs to be investigated rigorously.

4

The entanglement entropy of a bipartite quantum system is maximised by its corresponding thermofield double state, for a given β (see, for instance [39]). 5 This restricted access of a given observer to the observables of a subsystem, that commute with the observables of its complement, can be understood as having an information barrier between the two (in analogy with local observable algebras [32]).

1.2 Why Search for Quantum Gravity

5

1.2 Why Search for Quantum Gravity Presently our best description of nature is dichotomous and incomplete. Quantum matter is described by the standard model of particle physics, while classical gravity by general relativity. We are yet to discover a falsifiable theory that consistently merges a quantum theory of matter with gravitational phenomena, despite many advances in the various candidate approaches over the past decades [47, 48]. Gravity, by its very nature, responds to mass and energy, including quantum fields, i.e. quantum matter and gravity cannot be screened from each other. Thus, physical phenomena cannot be inherently divided into purely gravitational and quantum sectors. However the two separate theories, as they stand presently, do not accommodate this fact. Moreover, general relativity treats matter, which we know is fundamentally quantum, as classical. Therefore, if physics is to give a fully consistent and accurate account of our universe, then such a dichotomous description is incomplete at the very least, and certainly cannot reflect any fundamental separability between the quantum and gravitational regimes, even in principle. Thus, it seems that the physical world cannot be completely described by this disunified set of frameworks. [49, 50] Further, general relativity and quantum field theory are not valid at arbitrary energy scales. For instance in extreme environments, like the early universe or dynamical black holes, quantum fields will inevitably affect spacetime geometry to a significant extent and vice-versa. Also, even though we might not have data to which we can unambiguously assign a quantum gravitational origin, we certainly have phenomena that are still left unexplained by current theories, e.g. dark matter, dark energy, which could turn out to be low energy, non-perturbative effects of some underlying fundamental theory of quantum gravity. This further motivates the search for a unified framework [49–52], which is also expected to resolve divergences encountered in general relativity and quantum field theory [51, 52]. The path to quantum gravity may also shed light on the open foundational problem of time [51]. Time plays drastically different roles in quantum theory and general relativity [53–59]. The two notions are intrinsically incompatible within our present, limited understanding of the concept. In the context of conventional quantum theory, it plays the role of a global, external parameter characterising fully the evolution of a system. On the other hand in general relativity, both time and space are dynamical. In particular, the dynamics is constrained and coordinate time is gauge. It no longer carries the same physical status as that of a non-gravitational system (including relativistic field theories on a flat background). Similarly, a theory of quantum gravity may also be fundamentally ‘timeless’, in the sense that it may be devoid of an unambiguous notion of time, or may even display a complete absence of any time or clock variable. As we will see, the topic of this thesis, namely to develop a generalised framework for equilibrium statistical mechanics with subsequent applications in background independent discrete quantum gravity, is tightly linked with this issue. The notions of time, energy and temperature are inextricably intertwined. The search for a theory of quantum gravity is thus well-motivated and the need for it is largely acknowledged. But, what this theory is or could be, and how one should

6

1 Introduction

go about formulating it attracts numerous diverse methods and reasonings [47, 48], especially regarding which physical principles should be considered as foundational and indispensable to base the theory on. In this thesis, we are strictly concerned with fundamental discrete approaches to quantum gravity. Specifically, we work with the group field theory approach [60–66], which is a statistical field theory of candidate quanta of geometry of combinatorial and algebraic type [26, 67, 68], the same type of quanta that are utilised in several other discrete formalisms as will be discussed later.

1.3 Outline of the Thesis Background independence is a hallmark of general relativity that has revolutionised our conception of space and time. The picture of physical reality it paints is that of an impartial dynamical interplay between matter and gravitational fields. Spacetime is no longer a passive stage on which matter performs, but is an equally active performer in itself. Spacetime coordinates are gauge, thus losing their physical status of nonrelativistic settings. In particular, the notion of time is modified drastically. It is no longer an absolute, global, external parameter uniquely encoding the full dynamics. It is instead a gauge parameter associated with a Hamiltonian constraint. On the other hand, the well-established fields of quantum statistical mechanics and thermodynamics have been of immense use in the physical sciences. From early applications to heat engines and study of gases, to modern day uses in condensed matter systems and quantum optics, these powerful frameworks have greatly expanded our knowledge of physical systems. However, a complete extension of them to a background independent setting, such as that for a gravitational field, remains an open issue [26, 69–71]. The biggest challenge is the absence of an absolute notion of time, and thus of energy, which is essential to any standard statistical and thermodynamical consideration. This issue is particularly exacerbated in the context of defining statistical equilibrium, for the natural reason that the standard concepts of equilibrium and time are tightly linked. In other words, the constrained dynamics of a background independent system lacks a non-vanishing Hamiltonian in general, which makes formulating (equilibrium) statistical mechanics and thermodynamics, an especially thorny problem. This is a foundational issue, and tackling it is important and interesting in its own right. And even more so because it could provide useful insights into the very nature of fundamental quantum gravitational systems, and their connections with thermal physics. The importance of addressing these issues is further intensified in light of the open problem of emergence of spacetime in quantum gravity [1, 48, 72–74]. Having a quantum microstructure underlying a classical spacetime is a perspective that is shared, to varying degrees of details, by various approaches to quantum gravity such as loop quantum gravity (and related spin foams, and group field theories), simplicial gravity, and holographic theories, to name a few.

1.3 Outline of the Thesis

7

Specifically within discrete non-perturbative approaches, spacetime is replaced by more fundamental entities that are discrete, quantum and pre-geometric, in the sense that no notion of smooth metric geometry and continuum manifold exists yet. The collective dynamics of such quanta of geometry, governed by some theory of quantum gravity is then thought to give rise to an emergent spacetime, corresponding to specific phases of the full theory. For instance, in analogy with condensed matter systems, our universe can be understood as a kind of a condensate that is brought into the existing smooth geometric form by a phase transition of a quantum gravitational system of pre-geometric ‘atoms’ of space, with the cosmological evolution being encoded in effective dynamical equations for collective variables that are extracted from the underlying microscopic theory [30, 75–80]. Overall, this essentially entails identifying suitable procedures to extract a classical continuum from a quantum discretuum, and reconstructing effective general relativistic gravitational dynamics coupled with matter (likely with quantum corrections, potentially related to novel non-perturbative effects). This is the realm of statistical physics, which thus plays a crucial role even from the perspective of an emergent spacetime. The main technical strategy used in this thesis is to model discrete quantum spacetime as a many-body system [81], which in turn complements the view of a classical spacetime as a coarse-grained, macroscopic thermodynamic system. This formal suggestion is advantageous in multiple ways. It allows us to treat extended regions of quantum spacetime as built out of discrete building blocks, whose dynamics is determined by many-body mechanical models, here of generically non-local, combinatorial and algebraic type. It facilitates exploration of connections of discrete quantum geometries with quantum information theory and holography [17, 82–90]. Further, it makes possible implementing other many-body techniques, like algebraic Fock treatments and squeezing Bogoliubov transformations, for instance to find non-perturbative, possibly entangled vacua of the quantum gravitational system [46, 91, 92]. It also allows for the development of a statistical mechanical framework for these candidate quanta of geometry (here, of combinatorial and algebraic type), formally based on their many-body mechanics [25, 46, 68]. Such a framework naturally admits probabilistic superpositions of quantum geometries [25, 26, 68]; and facilitates studies of quantum gravitational states that incorporate fluctuations in relevant observables of the system, which can be interesting to study for example in the context of cosmology [46, 93–95]. This thesis is devoted to investigations of aspects like these. In particular, we illustrate, the potential of and preliminary evidence for, a rewarding exchange between a suitable background independent generalisation of equilibrium statistical mechanics, and discrete quantum gravity based on a many-body framework. These are the two facets of interest to us, to which our original contributions belong, as reported in [25, 26, 46, 68, 95, 96] and discussed in this thesis. Sections 2.2.4, 4.2.2.3 and 5.1.1.1, and Appendices 1 in Chap. 2, 1 in Chap. 4, 2 and 4 in Chap. 5, in this thesis include details that are not reported in our previous works.6 6 For [25]: Licensed under CC BY [creativecommons.org/licenses/by/3.0]. For [26, 46]: Licensed under CC BY [creativecommons.org/licenses/by/4.0]. For [68]: Reprinted excerpts and figures

8

1 Introduction

We begin in Chap. 2 with a discussion of a potential background independent extension of equilibrium statistical mechanics. In Sect. 2.1, we discuss the topic of presymplectic mechanics for many-body systems, in order to review the essentials to be utilised in later chapters, while also drawing attention to the role played by time in such systems. In Sect. 2.2.1, we clarify how to comprehensively characterise statistical states of the exponential Gibbs form, while placing the discussion within the broader context of the issue of background independent statistical equilibrium. After providing a succinct yet complete discussion of past proposals for generalised notions of statistical equilibrium in Sect. 2.2.2, we focus on the so-called thermodynamical characterisation for defining generalised Gibbs states in Sect. 2.2.3, which is based on a constrained maximisation of information entropy. In Sects. 2.2.4 and 2.2.5, we detail further crucial and favourable properties of this particular characterisation, also in comparison with the previously recalled proposals. Subsequently in Sect. 2.3, we discuss aspects of a generalised thermodynamics based directly on the generalised equilibrium setup derived above, including statements of the zeroth and first laws. This chapter presents a (partial) general framework, which forms the basis of our subsequent applications in discrete quantum gravity in the following chapters. In Chap. 3, we give an overview of the essentials of the many-body setup for the candidate quanta of geometry. The quanta considered here are combinatorial dvalent patches (elementary building blocks of graphs) dressed with algebraic data, which generate extended labelled graphs as generic boundary states. These types of states (dual to polyhedral complexes) are used in several discrete approaches, like loop quantum gravity, spin foams, group field theories and tensor models, dynamical triangulations and Regge calculus, which has motivated our choice of them also. Specifically in Sect. 3.4, we show that group field theories, in their covariant formulations in terms of field theory partition functions, arise as effective statistical field theories under a coarse-graining of a class of generalised Gibbs density operators of the underlying system of an arbitrarily large number of these quanta. A group field theory (GFT) thus being a field theory of such quanta, then its quantum operator formulation naturally offers a suitable route to a quantum statistical mechanical framework; or its associated many-body classical phase space formulation, to look into its corresponding classical statistical mechanics. This is the setting for our investigations in the subsequent chapters, by utilising the formalism of GFT. Now, GFTs are background independent, in the radical sense of spacetime-free approaches to quantum gravity. However, they also present specific peculiarities, which are crucial in various analyses, particularly in our development of an equilibrium statistical mechanical framework for them. The base space for the dynamical fields of GFTs consists of Lie group manifolds, encoding discrete geometric as well as matter degrees of freedom. This is not spacetime, and all the usual spatiotemporal features associated with the base manifold of a standard field theory are absent. As in with permission from [Goffredo Chirco, Isha Kotecha, and Daniele Oriti, Phys. Rev. D, 99, 086011, 2019. DOI: 10.1103/PhysRevD.99.086011]. Copyright 2019 by the American Physical Society. For [95]: Reprinted excerpts and figures with permission from [Mehdi Assanioussi and Isha Kotecha, Phys. Rev. D, 102, 044024, 2020. DOI: 10.1103/PhysRevD.102.044024]. Copyright 2020 by the American Physical Society. Minor modifications are made for better integration into this thesis.

1.3 Outline of the Thesis

9

other covariant systems, a physically sensible strategy for defining equilibrium can be to use internal dynamical variables, for example matter fields, as relational clocks with respect to which one defines dynamical evolution. Even in this case though, one does not expect the existence of a preferred material clock, nor, having chosen one, that this would provide a perfect clock, mimicking precisely an absolute Newtonian time coordinate. In the end, like standard constrained systems on spacetime, GFTs too are devoid of an external or even an internal variable that is clearly identified as a preferred physical evolution parameter. But the close-to-standard quantum field theoretic language used in GFTs, utilising many-body techniques in the presence of a base manifold (the Lie group, with associated metric and topology), imply the availability of some mathematical structures that are crucially shared with spacetimebased theories. This, then, allows us to move forward with the task of investigating their thermal aspects. In Chap. 4, we focus on the details of scalar group field theories, as required for the purposes of this thesis. In particular, we present the quantum operator formulation of bosonic GFTs associated with a degenerate vacuum i.e. a ‘no-space’ state, with no geometric and matter degrees of freedom, and detail the construction of its corresponding Fock representation in Sects. 4.1.1 and 4.1.2. Subsequently in Sects. 4.1.3 and 4.1.4, we provide an abstract Weyl algebraic formulation of the same system, and construct unitarily implementable translation automorphism groups. In Sects. 4.2.1 and 4.2.2, we address the issue of extracting a suitable clock variable, i.e. the issue of deparametrization in group field theory. In Chap. 5, we illustrate the applicability of the generalised statistical framework in discrete quantum gravity, based on the above many-body structure of GFTs. We present several concrete examples of classical and quantum generalised Gibbs states in Sect. 5.1. Then for the class of states associated with positive (semi-bounded in general, see Remark in Appendix 1 in Chap. 5) and extensive operator generators, we construct their corresponding class of inequivalent, thermal representations in Sect. 5.2, along with their non-perturbative thermal vacua. These cyclic vacua are thermofield double states, which we came across in Sect. 1.1 above. Our construction is based on the use of Bogoliubov transformation techniques from the field of thermofield dynamics. We further identify and construct an interesting class of states to describe thermal quantum gravitational condensates in Sect. 5.2.4. Equipped with these thermal condensates, we apply a specific kind of them, those which incorporate spatial volume fluctuations in quantum geometry, in the setting of GFT condensate cosmology in Sect. 5.3. For a free GFT model, we derive the effective dynamical equations of motion in terms of relational clock functions, in Sects. 5.3.2–5.3.4. Subsequently, we use these GFT equations of motion to derive relational generalised Friedmann equations, with quantum and statistical corrections, for homogeneous and isotropic cosmology in Sect. 5.3.5. At late times, we recover the correct classical limit; while at early times, we observe a bounce between a contracting and an expanding phase, along with an early phase of accelerated expansion featuring an increased number of e-folds compared to past studies of the same model. We conclude in Chap. 6 with a summary and outlook.

10

1 Introduction

References 1. Oriti D (2020) The Bronstein hypercube of quantum gravity. In: Matsubara K, Huggett N, Wüthrich C (eds) Beyond spacetime: the foundations of quantum gravity. Cambridge University Press 2. Bekenstein JD (1972) Black holes and the second law. Lett Nuovo Cim 4:737–740. https://doi. org/10.1007/BF02757029 3. Bekenstein JD (1973) Black holes and entropy. Phys Rev D 7:2333–2346. https://doi.org/10. 1103/PhysRevD.7.2333 4. Bekenstein JD (1974) Generalized second law of thermodynamics in black hole physics. Phys Rev D 9:3292–3300. https://doi.org/10.1103/PhysRevD.9.3292 5. Hawking SW (1975) Particle creation by black holes. Commun Math Phys 43:199–220. https:// doi.org/10.1007/BF01608497, https://doi.org/10.1007/BF02345020 6. Wall AC (2018) A survey of black hole thermodynamics. arXiv:1804.10610 7. Daniel H (2016) Jerusalem lectures on black holes and quantum information. Rev Mod Phys 88:015002. https://doi.org/10.1103/RevModPhys.88.015002 8. Carlip S (2014) Black hole thermodynamics. Int J Mod Phys D 23:1430023. https://doi.org/ 10.1142/S0218271814300237 9. ‘t Hooft G (1993) Dimensional reduction in quantum gravity. Conf Proc C930308:284–296 10. Susskind L (1995) The world as a hologram. J Math Phys 36:6377–6396. https://doi.org/10. 1063/1.531249 11. Jacobson T (1995) Thermodynamics of space-time: the Einstein equation of state. Phys Rev Lett 75:1260–1263. https://doi.org/10.1103/PhysRevLett.75.1260 12. Bardeen JM, Carter B, Hawking SW (1973) The four laws of black hole mechanics. Commun Math Phys 31:161–170. https://doi.org/10.1007/BF01645742 13. Bombelli L, Koul RK, Lee J, Sorkin RD (1986) A quantum source of entropy for black holes. Phys Rev D 34:373–383. https://doi.org/10.1103/PhysRevD.34.373 14. Srednicki M (1993) Entropy and area. Phys Rev Lett 71:666–669. https://doi.org/10.1103/ PhysRevLett.71.666 15. Ryu S, Takayanagi T (2006) Holographic derivation of entanglement entropy from AdS/CFT. Phys Rev Lett 96:181602. https://doi.org/10.1103/PhysRevLett.96.181602 16. Van Raamsdonk M (2010) Building up spacetime with quantum entanglement. Gen Rel Grav 42:2323–2329. https://doi.org/10.1142/S0218271810018529. [Int J Mod Phys D19:2429(2010)]. https://doi.org/10.1007/s10714-010-1034-0 17. Bianchi E, Myers RC (2014) On the architecture of spacetime geometry. Class Quant Grav 31:214002. https://doi.org/10.1088/0264-9381/31/21/214002 18. Jacobson T (2016) Entanglement equilibrium and the Einstein equation. Phys Rev Lett 116(20):201101. https://doi.org/10.1103/PhysRevLett.116.201101 19. Hoehn PA (2017) Reflections on the information paradigm in quantum and gravitational physics. J Phys Conf Ser 880(1):012014. https://doi.org/10.1088/1742-6596/880/1/012014 20. Van Raamsdonk M (2017) Lectures on gravity and entanglement. In: Proceedings, theoretical advanced study institute in elementary particle physics: new frontiers in fields and strings (TASI 2015): Boulder, CO, USA, June 1-26, 2015, pp 297–351. https://doi.org/10.1142/ 9789813149441_0005 21. Marolf D (2017) The Black Hole information problem: past, present, and future. Rept Prog Phys 80(9):092001. https://doi.org/10.1088/1361-6633/aa77cc 22. Jacobson T, Visser M (2019) Gravitational thermodynamics of causal diamonds in (A)dS. SciPost Phys 7(6):079. https://doi.org/10.21468/SciPostPhys.7.6.079 23. Jaynes ET (1957) Information theory and statistical mechanics. Phys Rev 106:620–630. https:// doi.org/10.1103/PhysRev.106.620 24. Jaynes ET (1957) Information theory and statistical mechanics. II. Phys Rev 108:171–190. https://doi.org/10.1103/PhysRev.108.171 25. Kotecha I, Oriti D (2018) Statistical equilibrium in quantum gravity: Gibbs states in group field theory. New J Phys 20(7):073009. https://doi.org/10.1088/1367-2630/aacbbd

References

11

26. Kotecha I (2019) Thermal quantum spacetime. Universe 5(8):187. https://doi.org/10.3390/ universe5080187 27. Jacobson T (2019) Entropy from Carnot to Bekenstein. In: Brink L, Mukhanov V, Rabinovici E, Phua KK (eds) Jacob Bekenstein: the conservative revolutionary, pp 73–87. https://doi.org/ 10.1142/9789811203961_0007 28. Bekenstein JD (1994) Do we understand black hole entropy? In: On recent developments in theoretical and experimental general relativity, gravitation, and relativistic field theories. Proceedings, 7th Marcel Grossmann Meeting, Stanford, USA, pp 39–58 29. Padmanabhan T (2010) Thermodynamical aspects of gravity: new insights. Rept Prog Phys 73:046901. https://doi.org/10.1088/0034-4885/73/4/046901 30. Padmanabhan T (2015) Emergent gravity paradigm: recent progress. Mod Phys Lett A 30(03n04):1540007. https://doi.org/10.1142/S0217732315400076 31. Marolf D, Minic D, Ross SF (2004) Notes on spacetime thermodynamics and the observer dependence of entropy. Phys Rev D 69:064006. https://doi.org/10.1103/PhysRevD.69.064006 32. Haag R (1992) Local quantum physics: fields, particles, algebras. Texts and monographs in physics. Springer, Berlin, Germany 33. Bratteli O, Robinson DW (1987) Operator algebras and quantum statistical mechanics. Vol 1: C* and W* algebras, symmetry groups, decomposition of states, 2nd edn. Springer, Berlin Heidelberg 34. Bratteli O, Robinson DW (1997) Operator algebras and quantum statistical mechanics. Vol 2: equilibrium states, models in quantum statistical mechanics, 2nd edn. Springer, Berlin Heidelberg 35. Kubo R (1957) Statistical mechanical theory of irreversible processes. 1. General theory and simple applications in magnetic and conduction problems. J Phys Soc Jap 12:570–586. https:// doi.org/10.1143/JPSJ.12.570 36. Martin PC, Schwinger JS (1959) Theory of many particle systems. 1. Phys Rev 115:1342–1373. https://doi.org/10.1103/PhysRev.115.1342 37. Haag R, Hugenholtz NM, Winnink M (1967) On the Equilibrium states in quantum statistical mechanics. Commun Math Phys 5:215–236. https://doi.org/10.1007/BF01646342 38. Takahasi Y, Umezawa H (1975) Thermo field dynamics. Collect Phenom 2:55–80. Reprint https://doi.org/10.1142/S0217979296000817 39. Khanna FC, Malbouisson APC, Malbouisson JMC, Santana AR (2009) Thermal quantum field theory - algebraic aspects and applications. World Scientific, New Jersey. http://ebooks. worldscinet.com/ISBN/9789812818898/9789812818898.html 40. Israel W (1976) Thermo field dynamics of black holes. Phys Lett A 57:107–110. https://doi. org/10.1016/0375-9601(76)90178-X 41. Unruh WG (1976) Notes on black hole evaporation. Phys Rev D 14:870. https://doi.org/10. 1103/PhysRevD.14.870 42. Bisognano JJ, Wichmann EH (1976) On the duality condition for quantum fields. J Math Phys 17:303–321. https://doi.org/10.1063/1.522898 43. Hartle JB, Hawking SW (1976) Path integral derivation of black hole radiance. Phys Rev D 13:2188–2203. https://doi.org/10.1103/PhysRevD.13.2188 44. Sewell GL (1982) Quantum fields on manifolds: PCT and gravitationally induced thermal states. Ann Phys 141:201–224. https://doi.org/10.1016/0003-4916(82)90285-8 45. Maldacena JM (2003) Eternal black holes in anti-de Sitter. JHEP 04:021. https://doi.org/10. 1088/1126-6708/2003/04/021 46. Assanioussi M, Kotecha I (2020) Thermal representations in group field theory: squeezed vacua and quantum gravity condensates. JHEP 20:173. https://doi.org/10.1007/JHEP02(2020)173 47. Kiefer C (2004) Quantum gravity. Int Ser Monogr Phys 124:1–308 48. Oriti D (2009) Approaches to quantum gravity: toward a new understanding of space, time and matter. Cambridge University Press. ISBN 9780521860451, 9780511512407. http://www. cambridge.org/catalogue/catalogue.asp?isbn=9780521860451 49. Huggett N, Callender C (2001) Why quantize gravity (or any other field for that matter)? Philos Sci 68(3):S382–S394. ISSN 00318248, 1539767X. http://www.jstor.org/stable/3080960

12

1 Introduction

50. Wüthrich C (2005) To quantize or not to quantize: Fact and folklore in quantum gravity. Philos Sci 72(5):777–788. ISSN 00318248, 1539767X. https://www.jstor.org/stable/10.1086/508946 51. Kiefer C (2007) Why quantum gravity? In: Stamatescu I-O, Seiler E (eds) Approaches to fundamental physics: an assessment of current theoretical ideas. Springer, Berlin Heidelberg, pp 123–130. ISBN 978-3-540-71117-9. https://doi.org/10.1007/978-3-540-71117-9_7 52. Nicolai H (2014) Quantum gravity: the view from particle physics. Fundam Theor Phys 177:369–387. https://doi.org/10.1007/978-3-319-06349-2_18 53. Anderson E (2012) Problem of time in quantum gravity. Annalen der Physik 524(12):757–786. https://doi.org/10.1002/andp.201200147 54. Höhn PA, Smith ARH, Lock MPE (2019) The trinity of relational quantum dynamics. https:// doi.org/10.1103/PhysRevD.104.066001 ˇ (2014) Quantum causality. Nat Phys 10(4):259–263. https://doi.org/10.1038/ 55. Brukner C nphys2930 56. Kiefer C (2017) Does time exist in quantum gravity? In: Lehmkuhl D, Schiemann G, Scholz E (eds) Towards a theory of spacetime theories. Springer, New York, pp 287–295. ISBN 9781-4939-3210-8. https://doi.org/10.1007/978-1-4939-3210-8_10 57. Rovelli C (2011) Forget time. Found Phys 41:1475–1490. https://doi.org/10.1007/s10701-0119561-4 58. Rovelli C (1991) Time in quantum gravity: an hypothesis. Phys Rev D 43:442–456. https:// doi.org/10.1103/PhysRevD.43.442 59. Wootters WK (1984) “Time” replaced by quantum correlations. Int J Theor Phys 23(8):701– 711. https://doi.org/10.1007/BF02214098 60. Reisenberger MP, Rovelli C (2001) Space-time as a Feynman diagram: the Connection formulation. Class Quant Grav 18:121–140. https://doi.org/10.1088/0264-9381/18/1/308 61. Freidel L (2005) Group field theory: an overview. Int J Theor Phys 44:1769–1783. https://doi. org/10.1007/s10773-005-8894-1 62. Oriti D (2007) Quantum gravity as a quantum field theory of simplicial geometry. In: Fauser B, Tolksdorf J, Zeidler E (eds) Quantum gravity: mathematical models and experimental bounds. Birkäuser Verlag, pp 101–126 63. Oriti D (2009) The group field theory approach to quantum gravity. In: Oriti D (ed) Approaches to quantum gravity: toward a new understanding of space, time and matter. Cambridge University Press 64. Oriti D (2011) The microscopic dynamics of quantum space as a group field theory. In: Proceedings, foundations of space and time: reflections on quantum gravity: Cape Town, South Africa, pp 257–320 65. Krajewski T (2011) Group field theories. PoS QGQGS2011(005). https://doi.org/10.22323/1. 140.0005 66. Oriti D, Ryan JP, Thuerigen J (2015) Group field theories for all loop quantum gravity. New J Phys 17(2):023042. https://doi.org/10.1088/1367-2630/17/2/023042 67. Oriti D (2016) Group field theory as the 2nd quantization of loop quantum gravity. Class Quant Grav 33(8):085005. https://doi.org/10.1088/0264-9381/33/8/085005 68. Chirco G, Kotecha I, Oriti D (2019) Statistical equilibrium of tetrahedra from maximum entropy principle. Phys Rev D 99(8):086011. https://doi.org/10.1103/PhysRevD.99.086011 69. Rovelli C (1993) Statistical mechanics of gravity and the thermodynamical origin of time. Class Quant Grav 10:1549–1566. https://doi.org/10.1088/0264-9381/10/8/015 70. Connes A, Rovelli C (1994) Von Neumann algebra automorphisms and time thermodynamics relation in general covariant quantum theories. Class Quant Grav 11:2899–2918. https://doi. org/10.1088/0264-9381/11/12/007 71. Rovelli C (2013) General relativistic statistical mechanics. Phys Rev D 87(8):084055. https:// doi.org/10.1103/PhysRevD.87.084055 72. Carlip S (2014) Challenges for emergent gravity. Stud Hist Phil Sci B 46:200–208. https://doi. org/10.1016/j.shpsb.2012.11.002 73. Oriti D (2014) Disappearance and emergence of space and time in quantum gravity. Stud Hist Phil Sci B46:186–199. https://doi.org/10.1016/j.shpsb.2013.10.006

References

13

74. Oriti D (2018) Levels of spacetime emergence in quantum gravity. arXiv:1807.04875 75. Hu BL (2005) Can spacetime be a condensate? Int J Theor Phys 44:1785–1806. https://doi. org/10.1007/s10773-005-8895-0 76. Oriti D (2017) The universe as a quantum gravity condensate. Comptes Rendus Physique 18:235–245. https://doi.org/10.1016/j.crhy.2017.02.003 77. Pithis AGA, Sakellariadou M (2019) Group field theory condensate cosmology: an appetizer. Universe 5(6). ISSN 2218-1997. https://doi.org/10.3390/universe5060147. https://www.mdpi. com/2218-1997/5/6/147 78. Gielen S, Sindoni L (2016) Quantum cosmology from group field theory condensates: a review. SIGMA 12:082. https://doi.org/10.3842/SIGMA.2016.082 79. Gabbanelli L, De Bianchi S (2021) Cosmological implications of the hydrodynamical phase of group field theory. Gen Relativ Gravit 53(7):66. https://doi.org/10.1007/s10714-021-02833-z 80. Gielen S (2014) Quantum cosmology of (loop) quantum gravity condensates: an example. Class Quant Grav 31:155009. https://doi.org/10.1088/0264-9381/31/15/155009 81. Oriti D (2018) Spacetime as a quantum many-body system. In: Angilella GGN, Amovilli C (eds) Many-body approaches at different scales: a tribute to norman h. march on the occasion of his 90th birthday. Springer International Publishing, Cham, pp 365–379. ISBN 978-3-31972374-7. https://doi.org/10.1007/978-3-319-72374-7_29 82. Colafranceschi E, Oriti D (2021) Quantum gravity states, entanglement graphs and secondquantized tensor networks. JHEP 07:052. https://doi.org/10.1007/JHEP07(2021)052 83. Chen Q, Livine ER (2021) Loop quantum gravity’s boundary maps. Class Quant Grav 38(15):155019. https://doi.org/10.1088/1361-6382/ac103f 84. Colafranceschi E, Chirco G, Oriti D (2021) Holographic maps from quantum gravity states as tensor networks. arXiv:2105.06454 85. Baytas B, Bianchi E, Yokomizo N (2018) Gluing polyhedra with entanglement in loop quantum gravity. Phys Rev D 98(2):026001. https://doi.org/10.1103/PhysRevD.98.026001 86. Livine ER (2018) Intertwiner entanglement on spin networks. Phys Rev D 97(2):026009. https://doi.org/10.1103/PhysRevD.97.026009 87. Chirco G, Mele FM, Oriti D, Vitale P (2018) Fisher metric, geometric entanglement and spin networks. Phys Rev D 97(4):046015. https://doi.org/10.1103/PhysRevD.97.046015 88. Chirco G, Goeßmann A, Oriti D, Zhang M (2020) Group field theory and holographic tensor networks: dynamical corrections to the Ryu-Takayanagi formula. Class Quant Grav 37(9):095011. https://doi.org/10.1088/1361-6382/ab7bb9 89. Chirco G, Oriti D, Zhang M (2018) Ryu-Takayanagi formula for symmetric random tensor networks. Phys Rev D 97(12):126002. https://doi.org/10.1103/PhysRevD.97.126002 90. Chirco G, Oriti D, Zhang M (2018) Group field theory and tensor networks: towards a RyuTakayanagi formula in full quantum gravity. Class Quant Grav 35(11):115011. https://doi.org/ 10.1088/1361-6382/aabf55 91. Kegeles A, Oriti D, Tomlin C (2018) Inequivalent coherent state representations in group field theory. Class Quant Grav 35(12):125011. https://doi.org/10.1088/1361-6382/aac39f 92. Bianchi E, Guglielmon J, Hackl L, Yokomizo N (2016) Squeezed vacua in loop quantum gravity. arXiv:1605.05356 93. Marchetti L, Oriti D (2021) Quantum fluctuations in the effective relational gft cosmology. Front Astron Space Sci 8:110. https://doi.org/10.3389/fspas.2021.683649 94. Gielen S, Oriti D (2018) Cosmological perturbations from full quantum gravity. Phys Rev D 98(10):106019. https://doi.org/10.1103/PhysRevD.98.106019 95. Assanioussi M, Kotecha I (2020) Thermal quantum gravity condensates in group field theory cosmology. Phys Rev D 102(4):044024. https://doi.org/10.1103/PhysRevD.102.044024 96. Chirco G, Kotecha I (2019) Generalized Gibbs ensembles in discrete quantum gravity. In: Nielsen F, Barbaresco F (eds) Geometric science of information 2019. Lecture notes in computer science (LNCS). Springer, Cham

Chapter 2

Generalised Statistical Equilibrium

Time is what keeps everything from happening at once. —Ray Cummings

What characterises statistical equilibrium? In a non-relativistic system, the answer is unambiguous. Equilibrium states are those which are stable under time evolution generated by the Hamiltonian H of the system. In the algebraic description, these are the states that satisfy the KMS condition [1–5]. For systems with finite number of degrees of freedom, KMS states take the explicit form of Gibbs states, whose density operators have the standard form, e−β H (see discussions in Appendix 2 in Chap. 5). This characterisation is unambiguous because of the special role of the time variable and its conjugate energy in standard statistical mechanics, where time is absolute, and modelled as the unique, external parameter encoding the dynamics of the system. Investigating this question in a background independent context, where the role of time is modified [6–11], is much more challenging and interesting. A complete framework for statistical mechanics in this setting is still missing. Classical gravity as described by general relativity (GR) is generally covariant. This means that space and time coordinates are gauge, and are not physical observables. Further, all geometric quantities, in particular temporal intervals, are dynamical, and generic solutions of the GR dynamics do not allow to single out any preferred time or space directions. This is the content of background independence in GR, and other modified gravity theories with the same symmetry content. Specifically, coordinate time is no longer a universal, physical evolution parameter. The absence of an unambiguous notion of time evolution is even more conspicuous in some quantum gravity formalisms in which an even more radical setup is invoked, where the familiar spatiotemporal structures of GR like the differential manifold, continuum metric, standard matter fields etc. have disappeared. How can one define an equilibrium thermal state then? © The Author(s), under exclusive license to Springer Nature Switzerland AG 2022 I. Kotecha, On Generalised Statistical Equilibrium and Discrete Quantum Gravity, Springer Theses, https://doi.org/10.1007/978-3-030-90969-7_2

15

16

2 Generalised Statistical Equilibrium

Covariant statistical mechanics [12–14] broadly aims at addressing the issue of defining a statistical framework for constrained systems on spacetime. This issue, especially in the context of gravity, was brought to the fore in [12], and developed subsequently in various studies of spacetime relativistic systems [12–18], valuable insights from which have also formed the conceptual backbone of our first applications to discrete quantum gravity [19–21]. In this chapter, we present (tentative) extensions of equilibrium statistical mechanics to background independent1 systems, laying out different proposals for a generalised statistical equilibrium, but emphasising on one in particular, based on which further aspects of a generalised thermodynamics are considered. In Sect. 2.1, we begin with a brief discussion surrounding the role of time in mechanics. The goal is not to give a thorough review of this vast subject of the nature and problem of time (see for example [6–9]), but to simply introduce the basic structures of classical constrained systems in terms of their presymplectic and extended phase space descriptions (to be utilised later in Sects. 4.2 and 5.1.2.2), and importantly, in the process, to bring to attention some specific features of constrained systems, particularly in the context of defining a suitable notion of statistical equilibrium for them. Since the notions of equilibrium and time are strongly linked, reconsidering the role of time in mechanics may guide us to understand better its role in statistical mechanics and thermodynamics, and in fundamental (even, spacetimefree) theories of quantum gravity.  In Sect. 2.2, we present generalised Gibbs states of the form e− a βa Oa . We begin in Sect. 2.2.1 with a detailed discussion of the defining characteristics of Gibbs states with the aim of generalising them to background independent systems [19]. In Sect. 2.2.2, we touch upon the various proposals for statistical equilibrium put forward in past studies on spacetime covariant systems [12, 14, 17, 22, 23], in order to better contextualise our work. In Sect. 2.2.3, we focus on the thermodynamical2 characterisation [19], based on Jaynes’ information-theoretic characterisation of equilibrium [24, 25]. We devote Sects. 2.2.4–2.2.5 to discuss various aspects of the thermodynamical characterisation, including highlighting many of its favourable features [20, 26], also compared to the other proposals. In fact, we point out how 1

In the earlier works mentioned above [12–18], such a framework is usually referred to as covariant or general relativistic statistical mechanics. But we will choose to call it background independent statistical mechanics as our applications to quantum gravity are evident of the fact that the main ideas and structures are general enough to be used in radically background independent systems devoid of any spacetime manifold or associated geometric structures and symmetries. 2 Using the terminology of [19], we call this a ‘thermodynamical’ characterisation of equilibrium, to contrast with the customary KMS condition’s ‘dynamical’ characterisation. For a detailed discussion of these, we refer to Sect. 2.2.1. The main idea is that the various proposals for generalised Gibbs states can be divided in terms of these two characterisations from an operational standpoint. Which characterisation one chooses to use in a given situation depends on the information or description of the system that one has at hand. For instance, if the description includes a 1-parameter flow of physical interest, then using the dynamical characterisation, i.e. satisfying the KMS condition with respect to it, will define statistical equilibrium with respect to it. The procedures defining these two characterisations can thus be seen as ‘recipes’ for constructing a Gibbs state, and which one is more suitable depends on our knowledge of the system.

2 Generalised Statistical Equilibrium

17

this characterisation can comfortably accommodate the past proposals for Gibbs equilibrium [26]. In Sect. 2.3, we define the basic thermodynamic quantities which can be derived immediately from a generalised Gibbs state, without requiring any additional physical and/or interpretational inputs. We clarify the issue of extracting a single common temperature for the full system from a set of several of them, and end with the zeroth and first laws of a generalised thermodynamics.

2.1 Rethinking Time in Mechanics Presymplectic mechanics is a powerful framework that is manifestly covariant, in the sense that it does not require non-relativistic concepts like absolute time to describe the physical dynamics of a system. It is used widely to describe dynamical systems which are generally covariant, or more generally are constrained systems with a set of gauge symmetries and a vanishing canonical Hamiltonian. In this section, we review the required details of the structure of classical, finite presymplectic systems, based primarily on discussions in [10, 19, 27–30], to be used subsequently in Sects. 4.2.1 and 5.1.2.2. Importantly, we draw attention to the role of time in mechanics, and re-emphasise the fact that it requires a rethinking in the context of background independence, especially in its connections to equilibrium statistical mechanics. In particular, we stress that time is what parametrizes a history, and this parametrization is neither absolute, nor global, nor non-dynamical in generic background independent settings. We discuss a reformulation of standard Hamiltonian mechanics in terms of a presymplectic system, which is then further described in terms of an extended symplectic phase space with the dynamics encoded in a Hamiltonian constraint. Using this simple class of standard Hamiltonian systems, which are equipped with a unique global notion of time, we illustrate the main features of a generic constrained particle system that is devoid of any such physical evolution parameter. We then move on to a brief discussion of deparametrization (i.e. a procedure to extract a clock variable, where there is none a priori), in order to anticipate the main ideas that will be encountered in the subsequent chapters in the context of quantum gravity. We will be succinct in our presentation, and focus mainly on the essential takeaways relevant for the topic of this thesis.

2.1.1 Preliminaries: Presymplectic Mechanics Hamiltonian Symplectic Mechanics Consider a non-relativistic dynamical system defined by, a symplectic space of states  equipped with a symplectic (closed, non-degenerate) 2-form ω, and a Hamiltonian

18

2 Generalised Statistical Equilibrium

H generating the time evolution αt , written together as (, ω, H ). By non-relativistic, we specifically mean that there exists a preferred, unique dynamical flow, denoted here by αt , encoding the complete physics of the system. In other words, there exists a physical evolution parameter, denoted here by t, which is unique, global and nondynamical (thus, external to the system), i.e. a Newtonian time. In this thesis, we deal with systems with an arbitrarily large, but finite, number of quanta. Thus, here also we are concerned with multi-particle systems with a finite total number. In the present section, for simplicity, we further restrict discussions to a single particle defined on a 1-dimensional smooth manifold C, which is its configuration space. This can be extended to a multi-particle system, and for a configuration space with a finite dimension greater than 1. Therefore, here (, ω, H ) describes a single classical particle, where  = T ∗ (C) is a cotangent bundle over the configuration space. Phase space  is a symplectic manifold with a symplectic 2-form ω. Local coordinates on C are (q), and correspondingly on  are (q, p). The symplectic form can be written using these coordinates as, ω = dp ∧ dq. The dynamics is encoded in a smooth, Hamiltonian function H :  → R. The equations of motion are given by, ω(X H ) = −d H

(2.1)

where the notation on the left hand side denotes the interior product of the symplectic 2-form with a vector field. This is a compact, geometric rewriting of Hamilton’s equations of motion, which can be seen as follows. The Hamiltonian vector field X H , as defined by the above equation, is given by X H = ∂ p H ∂q − ∂q H ∂ p

(2.2)

where, ∂q ≡ ∂/∂q denotes a partial derivative. Now, let t ∈ R parametrize the integral curves of X H on . Then, we get ∂p H =

dq(t) dp(t) , ∂q H = − dt dt

(2.3)

which are the Hamilton’s equations in a familiar form. Notice that the variable parametrizing the dynamical trajectories is what we call time (here, Newtonian). Parametrized Presymplectic Mechanics Let us parametrize the dynamical trajectories (q(t), p(t)) generated by H , and consider instead, graphs of them (t, q(t), p(t)), in an arbitrary parametrization (t (τ ), q(τ ), p(τ )). Then, these graphs are curves in the enlarged space  := R × , with local coordinates (t, q, p). We know that Eq. (2.1) encodes the dynamics on . Then on , this same dynamics takes the form, ω (X ) = 0

(2.4)

2.1 Rethinking Time in Mechanics

19

where, ω = ω − d H ∧ dt

(2.5)

is a closed, degenerate (presymplectic) 2-form on , and the vector field is proportional to, (2.6) X = ∂t + X H . Equation (2.4) means that X is a null vector field on . Its integral curves, called orbits,3 admit an arbitrary parametrization, denoted above by τ . Therefore, (, ω ) is a presymplectic manifold, and  is known as the constraint surface. Notice that Eqs. (2.1) ⇔ (2.4) (denoting, if and only if). In this sense, of having the same physical dynamics, the descriptions (, ω, H ) and (, ω ) with quantities as defined above, are equivalent for a non-relativistic Hamiltonian system. But for our purposes, what is important is to realise that the latter description allows for more generality, being able to also describe generic constrained systems. In fact, constrained systems admit a description of the former kind only if it is deparametrized, thus admitting a time or a clock structure. We will return to aspects of deparametrization shortly below, and later in Sects. 4.2 and 5.3.3. For now, let us introduce further extended structures, which will be of particular value to us in the context of classical group field theory in Sect. 4.2. Extended Symplectic Mechanics The main idea of the extended symplectic formulation is to take all relevant variables, including a time or a clock (if it is present), as being dynamical, thus subject to the dynamical constraint of the system. This is certainly a reasonable feature from an operational point of view, because any clock that one may use is made of matter, and is thus dynamical. For the case of a non-relativistic Hamiltonian system (, ω, H ), we have an extended configuration space Cex = R × C, along with the associated extended phase space ex = T ∗ (Cex ) = R2 ×  with local coordinates (t, pt , q, p). Evidently, time variable t is now internal to the system’s description. The symplectic structure on ex is, (2.7) ωex = ω + dpt ∧ dt and, the constraint function takes a specific form, given by C = pt + H (q, p) .

(2.8)

It is important to remark that this particular form of C, namely being first order in clock momentum and zeroth order in clock variable, is characteristic of having a dynamically viable clock or time structure. In other words, a system described by a 3 In general for k ≥ 1 number of scalar first class constraints, we have k-dimensional gauge orbits (null surfaces) on the constraint surface . See for instance [31], for details.

20

2 Generalised Statistical Equilibrium

constraint function of the above form is deparametrized, with a clock variable t. Also, when the constraint takes the form in Eq. (2.8), the presymplectic structure takes a specific form given by, ω = ω − d H ∧ dt, that we saw before. Furthermore in this case, the null vector field of ω is always of the form, XC = ∂t + X H

(2.9)

which is a direct consequence of the following crucial properties of the constraint function (in turn, arising as a direct consequence of its specific form in Eq. (2.8)), ∂C = 1, ∂ pt

∂C = 0. ∂t

(2.10)

We also see that the constraint surface in this case takes the form describing a foliation in t ∈ R, of the canonical phase space , that is  = R × .

(2.11)

Both, Eqs. (2.10) and (2.11), are characteristic of a system equipped with a good clock structure. In general, a constrained system is described by an extended configuration space Cex , extended phase space ex = T ∗ (Cex ) with a given symplectic 2-form ωex , and a smooth constraint function (2.12) C : ex → R which is not necessarily of the specific form in Eq. (2.8) above. If a given system is equipped with a clock variable, then it is now one of the configuration variables in Cex . However, existence of such a variable is not required for a well-defined description of the physical system. A constrained dynamical system in its extended description is thus given by (ex , ωex , C). Restricting to the surface where the constraint function vanishes gives the constraint surface,  = ex |C=0 ⊂ ex

(2.13)

which is not necessarily of the specific form in Eq. (2.11).  is a presymplectic manifold, with its degenerate 2-form defined via a pull-back, ω = ı ∗ ωex , of an embedding map ı :  → ex . The equations of motion are ω (XC ) = 0 .

(2.14)

Lastly, the reduced physical space, which is the space of orbits, can be obtained by factoring out the kernel of the presymplectic form. We thus have at hand three kinds of formulations for classical mechanical systems, namely: Hamiltonian symplectic (, ω, H ), presymplectic (, ω ), and extended symplectic (ex , ωex , C). For non-relativistic systems, or more generally for systems

2.1 Rethinking Time in Mechanics

21

characterised by a Hamiltonian constraint of the form (2.8), these three are all equivalent. But importantly, only the last two are general enough for generic background independent systems, since their description of the dynamics does not rely on the choice, or even the existence, of an explicit time evolution variable.

2.1.2 Deparametrization Given a constrained system (ex , ωex , C), we have stressed above that its description may not necessarily include a good clock structure. And that even without such a structure, the extended (or presymplectic) formulation describes fully the dynamical system. In such a priori ‘timeless’ systems then, we may still want to extract a clock variable. This is called deparametrization. In the present context for instance, deparametrization is valuable to define physical equilibrium states with respect to clock Hamiltonians (see Sects. 2.2.1, 2.2.2 and 5.1.2.2 for more discussions and examples). From the above discussions of constrained mechanical systems, especially in comparison with extended non-relativistic systems, we can identify the core, universal strategy behind deparametrization: to reformulate, either exactly or under certain approximations, the dynamical constraint of the system, to bring it to the form of Eq. (2.8), i.e. (2.15) C −→ Cdep = pλ + H (qcan , pcan ) where λ is the clock variable, H is the clock Hamiltonian generating evolution in clock time λ, and (qcan , pcan ) denote the phase space variables of the canonical system to which the clock variable is external. A simple illustrative example is a classical relativistic particle on spacetime, with its covariant dynamics given by, C = p2 − m 2 ,

(2.16)

which is defined on an extended phase space ex coordinatised by (x μ , pμ ), with μ = 0, 1, 2, 3 and signature (+, −, −, −). In this case, the complete dynamical, presymplectic description does not require deparametrization, i.e. given the extended phase space along with C, its constraint surface is well-defined. But the point is that this system is deparametrizable, which means that it is possible to bring C to a manifestly non-covariant form, here without changing the physics that is captured completely by the constraint surface (, ω ). The full constraint can be rewritten as Cdep = p0 +



p2 + m 2

(2.17)

22

2 Generalised Statistical Equilibrium

which now describes the same relativistic particle system but in a fixed Lorentz frame and the where the configuration variable x 0 has been chosen as the clock variable  corresponding clock dynamics is dictated by the Hamiltonian H = p2 + m 2 . A different example of a system which by itself is non-deparametrizable, i.e. it doesn’t naturally admit a good clock without further approximations, is the so-called timeless double pendulum [10, 28, 32]. It is defined by an extended configuration space Cex = R2  (q1 , q2 ), phase space ex = T ∗ (Cex ) with ωex =  a 4 a=1,2 dpa ∧ dq , and a dynamical constraint C=

1 2 (q + q22 + p12 + p22 ) − k 2 1

(2.18)

for a real constant k.√The constraint surface in this case is,  = ex |C=0 ∼ = S3, a 3-sphere with radius 2k. Clearly,  is compact and does not admit a form (2.11) with a foliation that is characteristic of having a time structure. Therefore, the system so described does not naturally have any internal variable which can play the role of time, before any approximations. For instance, if one were to approximate the dynamics by the following constraint function, 1 Cdep = p2 + (q12 + p12 ) − k ≡ p2 + H (q1 , p1 ) 2

(2.19)

then, in this dynamical regime (if it exists) described by Cdep , variable q2 acts as a good clock parameter with the physical evolution being generated by H . Finally, we note that in the case of a system composed of many particles, there may not exist a single global clock, even if each particle is deparametrized separately and thus equipped with its own individual clock. In this case then, one would expect to have to sync the different clocks in order to define a single common clock. This issue can be investigated in a general multi-particle setting, continuing from the discussions above [15, 18]. However, we will discuss it in detail directly in the context of classical GFTs [19] in Sect. 4.2.1.

2.2 Generalised Gibbs Equilibrium Equilibrium states are a cornerstone of statistical mechanics and thermodynamics. They are vital in the description of macroscopic systems with a large number of microscopic constituents. In particular, Gibbs states have a vast applicability across a broad range of fields such as condensed matter physics, quantum information, tensor networks, and (quantum) gravity, to name a few. They are special, being the 4

Notice that this system is fundamentally different from an analogous, non-relativistic one with Newtonian time t, which would instead be given by a constraint of the form, C = pt + 21 (q12 + q22 + p12 + p22 ) − k.

2.2 Generalised Gibbs Equilibrium

23

unique class of states in finite systems satisfying the KMS condition.5 Furthermore, usual coarse-graining techniques also rely on the definition of Gibbs measures. In treatments closer to hydrodynamics, one often considers the full (non-equilibrium) system as being composed of many interacting subsystems, each considered to be at local equilibrium. While in the context of renormalisation group flow treatments, each phase at a given scale, for a given set of coupling parameters is also naturally understood to be at equilibrium, each described by (an inequivalent) Gibbs measure. Given this physical interest in Gibbs states, the question then is how to define them for background independent systems.

2.2.1 Characterising Gibbs States Let us begin with a discussion on how to characterise completely statistical states of the Gibbs form, based on insights from both standard and covariant statistical mechanics [19]. This discussion is not restricted to any particular quantum gravity formalism, or even to classical or quantum sectors for systems on spacetime. Rather, it attempts to present the strategies employed in past studies for defining Gibbs states, along with a variety of examples, in a coherent way. The main goal here is to reconsider the standard characterisations that are well-known to us, and attempt to understand them from a broader perspective, in order to then generalise them to background independent systems, including discrete quantum gravity. Gibbs states, ρβ = Z1β e−βO (where O is not necessarily a Hamiltonian), can be categorised according to two main criteria, respectively primary and secondary: A. whether or not the state is a result of considering an associated pre-defined flow or transformation of the system; B. the nature of the functions or operators O in the exponent characterising the state, specifically whether these quantities encode the physical dynamics of the system, or refer to some structural properties. Categories A and B are mutually independent, in the sense that a single system could simultaneously be both of types A and B. Details of these two categories, their respective subclasses and related examples follow. Let us first look at the primary category A, which can be considered at a higher footing than the secondary B because the contents of classification under A are the actual construction procedures or ‘recipes’ used to arrive at a resultant Gibbs state. 5

The algebraic KMS condition [4, 5] is known to provide a comprehensive characterisation of statistical equilibrium in systems of arbitrary sizes, as long as there exists a well-defined 1-parameter dynamical group of automorphisms of the system. This latter point, of the required existence of a preferred time evolution of the system, is exactly the missing ingredient in generic background independent cases. Moreover, we observe that the automorphism group in the definition of KMS condition does not, technically, need to be identified with time evolution. Thus KMS equilibrium can be defined for more general symmetries, even though the standard definition would be physically more natural in systems with a unique definition of time. We refer to Sects. 2.2.1 and 2.2.5 for more details.

24

2 Generalised Statistical Equilibrium

Moreover, it is within A where we observe that the known Jaynes’ entropy maximisation principle [24, 25] could prove to be especially useful in background independent contexts such as in discrete quantum gravity frameworks. Under A, we can identify two recipes to construct, or equivalently, ways to completely characterise, a Gibbs state depending on the information that we have at hand for a given system. A1. Dynamical Characterisation: Use of Kubo-Martin-Schwinger Condition The KMS condition [1–5] is formulated in terms of a 1-parameter group of automorphisms of the system. Let ω be an algebraic state6 over a C*-algebra7 A, and αt be a 1-parameter group of *-automorphisms8 of A. Consider the strip I = {z ∈ C | 0 < Im(z) < β, β ∈ R≥0 }, and let I¯ denote its closure, such that I¯ = R if β = 0. Then, ω is an α-KMS state at value β, if for any pair A, B ∈ A, there exists a complex function FAB (z) which ¯ such that it satisfies the KMS is analytic on I, and continuous and bounded on I, boundary conditions: FAB (t) = ω[A αt (B)] ,

FAB (t + iβ) = ω[αt (B) A]

(2.20)

for all t ∈ R [5]. We note that an α-KMS state satisfies stationarity, i.e. ω[αt A] = ω[A] (for all t), which captures the simplest notion of equilibrium (see Appendix 2 in Chap. 5 for some more details). If in the given description of a system, one can identify a relevant set of transformations (not necessarily Hamiltonian) with respect to which one is interested in defining an equilibrium state, then one asks for the state to satisfy the KMS condition with respect to a continuous, unitarily implementable 1-parameter (sub-) group of the said transformations. This gives (uniquely, for a certain class of systems as detailed in Appendix 2 in Chap. 5, e.g. finite systems on spacetime), a Gibbs state of the form ρ ∝ e−βG , where G is the self-adjoint generator of the flow, and β ∈ R. Notice that the ‘inverse temperature’ β enters formally as the periodicity in the flow parameter t, regardless of its interpretation. Thus, this characterisation is strictly based on the existence of a suitable predefined flow of the configurations of the system and then imposing the KMS condition with respect to it. These transformations could correspond to physical or structural properties of the system (see category B below). Simple examples are, respectively, Algebraic states ω : A → C, are complex-valued, linear, positive, normalised functionals over an algebra. Linearity is: ω[z 1 A + z 2 B] = z 1 ω[A] + z 2 ω[B] ∀z 1 , z 2 ∈ C. Positivity is: ω[A† A] ≥ 0 ∀A ∈ A. Normalisation is: ω[I ] = 1, where I is the identity element of A [33]. 7 A C*-algebra is a norm complete *-algebra, equipped with the C*-norm property: ||A∗ A|| = ||A||2 . A normed *-algebra is a *-algebra equipped with a *-norm. A *-algebra is an algebra (i.e. vector space over C, with an associative and distributive multiplication law) equipped with a *operation (also called, involution or adjoint) such that: A∗∗ = A, (AB)∗ = B ∗ A∗ , and (z 1 A + z 2 B)∗ = z¯ 1 A∗ + z¯ 2 B ∗ . A *-norm is a norm ||.|| with one additional property: ||A∗ || = ||A||. We note that in this thesis, we denote the *-operation by a dagger † [33]. 8 A *-automorphism is a bijective *-homomorphism of the algebra into itself. We refer to Appendix 1 in Chap. 4 for details [33]. 6

2.2 Generalised Gibbs Equilibrium

25

the physical time flow ei H t in a non-relativistic system where H is the Hamiltonian, which gives rise to the standard Gibbs equilibrium state of the form e−β H ; and a U (1) gauge flow ei N θ where N is a number operator, which would lead to an equilibrium state of the form e−β N . A2. Thermodynamical Characterisation: Use of Maximum Entropy Principle Under a Given Set of Constraints Consider a situation wherein the given description of a system does not include relevant symmetry transformations, or (even if such symmetries exist, which they usually do) that we are interested in those properties of the system which are not naturally associated to sensible flows, in the precise sense of being generators of these flows. Examples of the latter are observables such as area, volume or mass. Geometric operators like volume are of special interest in the context of quantum gravity since they may be instrumental for statistically extracting macroscopic geometric features of spacetime regions from quantum gravity microstates. In such cases then, what characterises a Gibbs state and what is the notion of equilibrium encoded in it? In order to construct a Gibbs state here, where operationally we may only have access to a set of constraints fixing the mean values of a set of functions or operators {Oa ρ = Oa }a=1,2,..., (in classical or quantum descriptions respectively), one must rely on Jaynes’ principle [24, 25] of maximising the entropy S[ρ] = −ln ρρ while simultaneously satisfying the above constraints. The angular brackets denote statistical averages in a state ρ defined on the state space of the system, be it a phase space in the classical description or a Hilbert space inthe quantum one. Undertaking this procedure, one arrives at a Gibbs state ρ = e− a βa Oa (where one of the O’s is the identity fixing the normalisation of the state as will be detailed below in Sect. 2.2.3). We can see that here the inverse temperatures βa enter formally as Lagrange multipliers. Also, the averages Oa with parameters βa , and other quantities derived from them, can be understood as thermodynamic variables defining a macrostate of the system, and can take on the same formal roles as in usual statistical mechanics and thermodynamics. But their exact interpretation would depend on the context. The identification and interpretation of such relevant quantities is in fact the non-trivial aspect of the problem, particularly in quantum gravity. Notice that this characterisation is strictly independent of the existence of any predefined transformations or symmetries of the underlying microscopic system, as long as there is at least one function or operator (identified as relevant) whose statistical average is assumed (or known) to be fixed at a certain value. Consequently, this characterisation could be most useful in background independent settings, exactly since it is based purely on Jaynes’ information-theoretic method. Finally, we note that in this characterisation a notion of equilibrium is implicit in the requirement that a certain set of observable averages remain constant, i.e. it is implicit in the existence of the constraints Oa ρ = Oa (see for example the discussion in section II in [34]). We will undertake a detailed discussion of the thermodynamical characterisation,

26

2 Generalised Statistical Equilibrium

and formulate aspects of a generalised equilibrium statistical mechanical framework based on it, along with basic features of its generalised thermodynamics, in the remaining sections of this chapter. For now, let us summarise the above classifications and make some additional remarks. If the aim is to construct Gibbs states for a system of many quanta (whatever they may be), then the two characterisations, dynamical and thermodynamical, under category A offer us two formally independent strategies to do so. Based on our knowledge of a given system, we may prefer to use one over the other. If there is a known set of symmetries with respect to which one is looking to define equilibrium, then the technical route one takes is to construct a state satisfying the KMS condition with respect to (a 1-parameter subgroup of) the symmetry group. The result of using this recipe in a finite system (cf. remarks in Appendix 2 in Chap. 5) is a Gibbs state e−βG , characterised by the generator G of the 1-parameter flow of these transformations and the periodicity parameter β. On the other hand, if one does not have interest in or access to any particular symmetry transformations of the system, but has a partial knowledge about the system in terms of a set of observable averages Oa , then one employs the principle of maximising Shannon or von Neumann entropy under the given set ofconstraints. The resultant statistical state is again of a Gibbs exponential form e− a βa Oa , now characterised by the set of observables Oa and Lagrange multipliers βa . Notice that given a Gibbs state, constructed say from recipe A1, then once it is already defined, it also satisfies the thermodynamic condition of maximum entropy [4, 5]. Similarly, a Gibbs state defined on the basis of A2, after it is constructed also satisfies the KMS condition with respect to a flow that is derived from the state itself (due to Tomita-Takesaki theorem [4, 5]). For instance, consider the standard nonrelativistic Gibbs state e−β H , which is constructed by satisfying the KMS condition with respect to unitary time translations ei H t . That is, this state is classified as A1 since its construction relies on the KMS condition. But, once this state is defined, it is also the one that maximises the entropy under the constraint H  = E. Now consider an example of a state e−βV , where V is say spatial volume. This state is derived as a result of maximising the information entropy under the constraint V  = v, hence it is classified as A2. Once this state is defined, one can extract a flow from the state, with respect to which it will satisfy the KMS condition.9 This is the modular flow eiβV τ , where τ is the modular flow parameter.10 Therefore, classifications A1 and A2 refer to the construction procedures employed as per the situation at hand. Once a Gibbs state is constructed using any one of the two procedures, then technically it

9

In the context of covariant statistical mechanics, the utility of this observation has been presented in [12–14], and is the crux of the thermal time hypothesis. 10 In a classical phase space description of a system, the modular flow is the integral curve of the vector field XV defined by ω(XV ) = −d V , where ω is the symplectic form and V is a smooth function. In this case naturally the flow eτ XV is in terms of the vector field XV = ∂τ . In the quantum C*-algebraic description (or in a specific Hilbert space representation of it), the modular flow is that of the Tomita-Takesaki theory.

2.2 Generalised Gibbs Equilibrium

27

will satisfy both the KMS condition with respect to a flow,11 and maximisation of entropy. Now, given that a Gibbs state can be constructed as a result of either the dynamical or the thermodynamical recipe, one can consider the nature of the functions or operators O that characterise it. This is the content of classification under category B. B1. Physical State If O is associated with the physical dynamics of the system, i.e. it dictates, partially or completely, the dynamical model of the system, then the associated Gibbs state can be understood as encoding, partially or completely, a physical notion of equilibrium. In a standard non-covariant system, O would simply be the Hamiltonian. While in a covariant system, if it is deparametrizable with a suitable choice of a good clock, then O would be the associated clock Hamiltonian. Overall, this particular classification refers explicitly, and in the definition of the Gibbs state, to the physical dynamical evolution of the system. This is encoded in a relevant model-dependent function or operator, whether it is a conventional Hamiltonian or a deparametrizable constraint. B2. Structural State If O are quantities referring to kinematic or structural properties of the system, and not directly to the specific physical dynamical model of it, then the associated Gibbs states are understood to be structural. Examples of structural transformations are generic rotations or translations of the base manifold of the theory. Examples of quantities that are not necessarily associated to symmetry transformations would be observables like area or volume. Examples Four different types of Gibbs states can be constructed from combinations of classifications under categories A and B. Let us mention a variety of examples, including the ones constructed as part of this thesis. A1–B1: Gibbs states with respect to physical time translations, as considered in standard statistical mechanics [4, 5, 35]; with respect to a clock time in deparametrized systems, with examples constructed in covariant statistical mechanics on spacetime [14, 18, 22] (Sect. 2.2.2), and in group field theory quantum gravity [19] (Sect. 5.1.2.2). A2–B1: Gibbs states with respect to 4-momenta of relativistic particles in covariant statistical mechanics [17]; with respect to momentum map associated with diffeomorphism group for parametrized field theory [36, 37]; with respect to a dynamical projector [20, 21, 38], and kinetic and vertex operators [26] in group field theory (Sect. 3.4). 11

Whether the flow parameter has a reasonable physical interpretation is a separate issue, and would depend on the specific context.

28

2 Generalised Statistical Equilibrium

A1–B2: Gibbs states with respect to U(1) symmetry generated by the number observable in standard statistical mechanics [4, 5, 35]; with respect to internal translation automorphisms in algebraic group field theory [19] (Sect. 5.1.2.1). A2–B2: Souriau’s Gibbs states with respect to kinematical symmetries [29, 39]; Gibbs states with respect to gauge-invariant observables in covariant statistical mechanics on spacetime [17]; with respect to spatial volume for pressure ensemble in standard statistical mechanics [24]; with respect to geometric area and volume operators in loop quantum gravity [17, 40]; with respect to positive, extensive operators in group field theory, e.g. spatial volume operator [19] (Sect. 5.1.1); with respect to classical closure and half-link gluing constraints in group field theory [20, 21] (Sect. 5.1.3). In light of the fact that these classifications comprehensively span all possible kinds of Gibbs states, we call them generalised Gibbs states.

2.2.2 Past Proposals We now give an overview [26] of the different proposals for defining statistical equilibrium based on studies in covariant statistical mechanics, in order to better contextualise our proposal of the thermodynamical characterisation which is the focus of the subsequent sections. These proposals rely on various different principles originating in standard non-relativistic statistical mechanics, extended to a constrained setting. The first proposal [12, 15] was based on the idea of statistical independence of arbitrary (small, but macroscopic) subsystems of the full system, in a classical setting. The notion of equilibrium is taken to be characterised by the factorisation property of the state, (2.21) ρ = ρ1 ρ2 for any two subsystems 1 and 2; and where ρ1 and ρ2 are taken to be defined on mutually exclusive subregions of the full phase space, so that we additionally have {ρ1 , ρ2 } = 0 ,

(2.22)

[Xρ1 , Xρ2 ] = 0 ,

(2.23)

or equivalently, where, ω(Xρ1,2 ) = d ln ρ1,2 , ω is the symplectic form on the phase space of the full system, and {., .} is the Poisson bracket. Then, the whole system is said to be at equilibrium if any one of its subsystems is statistically independent from all the rest. We note that this characterisation for equilibrium is related to an assumption of weak interactions [35].

2.2 Generalised Gibbs Equilibrium

29

This same dilute gas assumption is integral also to the Boltzmann method of statistical mechanics. It characterises equilibrium as the most probable distribution, that is one with maximum entropy. This method is used in [17] to study a gas of constrained particles.12 Even though this method relies on maximising the entropy like the thermodynamical characterisation, it is more restrictive than the latter, as will be made clear in Sect. 2.2.5. The work in [14] puts forward a characterisation for a physical equilibrium state. The suggestion is that, ρ (itself a well-defined state on the physical, reduced state space) is said to be a physical Gibbs state if (i) its modular Hamiltonian h = − ln ρ ,

(2.24)

is a smooth function on the physical state space, and (ii) h is such that there exists a (local) clock function T (x) on the extended state space, with its conjugate momentum pT (x), such that h is proportional to pT . Importantly, when this is the case the modular flow (‘thermal time’ [12, 13]) is a geometric flow foliating spacetime, in which sense ρ is said to be ‘physical’. Notice that the built-in strategy here is to define KMS equilibrium in a deparametrized system, since by construction it identifies a state’s modular Hamiltonian with a (local) clock Hamiltonian on the base spacetime manifold. Thus it is an example of using the dynamical characterisation, associated with a clock Hamiltonian in a deparametrized system with constraint of the form (2.8). Another strategy [22] is based on the use of the ergodic principle and introduction of clock subsystems to define clock time averages. This characterisation relies on the validity of a postulate, even if traditionally a fundamental one, like two of the previous ones that were based on the physical assumption of weak interactions. Finally, the proposal in [23] interestingly characterises equilibrium by a vanishing information flow between interacting histories. The notion of information used is that of Shannon (entropy), I = ln N , (2.25) where N is the number of microstates traversed in a given history during interaction. Equilibrium between two histories 1 and 2 is encoded in a vanishing information flow, (2.26) δ I = I2 − I1 = 0 . This characterisation of equilibrium is evidently information-theoretic, even if relying on an assumption of weak interactions. Moreover it is much closer to our thermodynamical characterisation, because the condition of vanishing δ I is nothing but an optimisation of information entropy. These different proposals, along with the thermal time hypothesis [12, 13], have led to some remarkable results, like recovering the Tolman-Ehrenfest effect [16, 12

We remark that except for this one work, all other studies in spacetime covariant statistical mechanics are carried out from the Gibbs ensemble point of view.

30

2 Generalised Statistical Equilibrium

18], relativistic Jüttner distribution [18] and Unruh effect [41]. However, they all assume the validity of one or more principles, postulates or assumptions about the system. Moreover, none (at least presently) seems to be general enough like the proposal below, so as to be implemented in a full quantum gravity setup, while also accommodating within it the rest of the proposals.

2.2.3 Thermodynamical Characterisation This brings us to the proposal of characterising a generalised Gibbs state based on a constrained maximisation of information (Shannon or von Neumann) entropy [19– 21, 26], along the lines advocated by Jaynes [24, 25] purely from the perspective of evidential statistical inference. Jaynes’ approach is fundamentally different from other more traditional ones of statistical physics. So too is the thermodynamical characterisation, compared with the others outlined above, as will be exemplified in the following. It is thus a new proposal for background independent equilibrium [19, 42], which has the potential of incorporating also the others as special cases, from the point of view of constructing a Gibbs state [26]. Consider a macroscopic system with a large number of constituent microscopic degrees of freedom. Our (partial) knowledge of its macrostate is given in terms of a finite set of averages {Oa  = Ua } of the observables that we have access to. Jaynes suggests that a fitting probability estimate (which, once known, will allow us to infer also the other observable properties of the system) is not only one that is compatible with the given observations, but also that which is least-biased in the sense of not assuming any more information about the system than what we actually have at hand, namely {Ua }. In other words, given a limited knowledge of the system (which is always the case in practice for any macroscopic system), the least-biased probability distribution compatible with the given data should be preferred. As shown below, this turns out to be a Gibbs distribution with the general form (2.31), which we refer to as generalised Gibbs states. Let  be a symplectic phase space (be it extended or reduced), which is a cotangent bundle over a finite-dimensional, smooth configuration manifold. Consider a finite set of smooth real-valued functions Oa defined on , with a = 1, 2, . . . , . Denote by ρ a smooth statistical density (real-valued, positive and normalised function) on , to be determined. Then, the prior on the known macrostate gives a finite number of constraints,  dλ ρ Oa = Ua , (2.27) Oa ρ = 

along with the normalisation constraint for the state, 1ρ = 1 ,

(2.28)

2.2 Generalised Gibbs Equilibrium

31

where dλ is a Liouville measure on , and the integrals are taken to be well-defined. Further, ρ has an associated Shannon entropy S[ρ] = −ln ρρ .

(2.29)

By understanding S to be a measure of uncertainty quantifying our ignorance about the details of the system, the corresponding bias is minimised (compatibly with the prior data) by maximising S (under the set of constraints (2.27) and (2.28)) [24]. Using the Lagrange multipliers technique, this amounts to finding a stationary solution for the following auxiliary functional L[ρ, βa , κ] = S[ρ] −



βa (Oa ρ − Ua ) − κ(1ρ − 1)

(2.30)

a=1

where βa , κ ∈ R are Lagrange multipliers. Then, requiring stationarity13 of L with respect to variations in ρ gives a generalised Gibbs state ρ{βa } =

1 Z {βa }

e

−



βa Oa

(2.31)

a=1

with partition function,  Z {βa } ≡

dλ e−

 a

βa Oa



= e1+κ ,

(2.32)

where as is usual, normalisation multiplier κ is a function of the remaining multipliers. The partition function Z {βa } encodes all properties of the system in principle. Analogous arguments hold for quantum mechanical systems and the above scheme can be implemented directly [25], as long as the operators under consideration are such that the relevant traces are finite on a representation Hilbert space. Statistical states are density operators (self-adjoint, positive, and trace-class operators, with Tr(ρ) = 1) on the Hilbert space. Statistical averages for (self-adjoint) observables Oˆ a are now, (2.33) Oˆa ρ = Tr(ρˆ Oˆ a ) = Ua . Following the constrained optimisation method again gives a Gibbs density operator, ρˆ{βa } = 13

1 Z {βa }

e

−

 a=1

βa Oˆ a

.

(2.34)

Notice that requiring stationarity of L with variations in the Lagrange multipliers implies fulfilment of the constraints (2.27) and (2.28). These two ‘equations of motion’ of L along with the one determining ρ (coming from stationarity of L with respect to ρ) provide a complete description of the system at hand.

32

2 Generalised Statistical Equilibrium

A generalised Gibbs state can thus be defined, characterised fully by a finite set of observables of interest Oa , and their conjugate generalised ‘inverse temperatures’ βa . Given this class of equilibrium states, it should be evident that some thermodynamic quantities (like generalised ‘energies’ Ua ) can be identified immediately. Aspects of a generalised thermodynamics will be discussed in Sect. 2.3. We note that there are two key features of this characterisation. First is the use of evidential (epistemic) probabilities, thus taking into account the given evidence {Ua }. This interpretation, that statistical states are states of knowledge [43–45], is innate to Jaynes’ method [24, 25]. Second is a preference for the least-biased (or most “honest”) distribution out of all the different ones compatible with the given evidence. It is not enough to arbitrarily choose any that is compatible with the prior data. An aware observer must also take into account their own ignorance, or lack of knowledge honestly, by maximising the information entropy.

2.2.4 Modular Flows and Stationarity Given a generalised Gibbs state, a natural question that arises is, with respect to which flow or transformations of the system is this state stationary. We know that any density distribution or operator is stationary with respect to its own modular flow. In fact by the Tomita-Takesaki theorem [4, 5], any faithful algebraic state over a von Neumann algebra is KMS with respect to its own 1-parameter modular (Tomita) flow. In the classical case then, a generalised Gibbs state ρ{βa } of the form (2.31), is stationary with respect to the local flow etXρ (parametrized by t ∈ R) on a given symplectic phase space , generated by vector field Xρ that is defined by the equation ω(Xρ ) = −dh ,

(2.35)

where h is the modular Hamiltonian of the state,  βa Oa . h=

(2.36)

a

Then, stationarity with respect to the modular flow is evident from, Xρ (ρ{βa } ) = {ρ{βa } , h} = 0

(2.37)

where, {., .} is a Poisson bracket on the algebra of smooth functions over . Now, the individual flows generated by Xa are associated with the different observables via the defining equation (2.38) ω(Xa ) = −dOa .

2.2 Generalised Gibbs Equilibrium

33

Then, we have that the modular vector field is in general a linear superposition of the separate ones, weighted by their respective inverse temperatures, Xρ =



βa Xa

(2.39)

a

using Eqs. (2.35), (2.38), and, linearities of the symplectic form ω and the exterior derivative. In particular, ρ{βa } is not stationary in general with respect to the individual flows Xa  generated by Oa  , that is Xa  (ρ{βa } ) = {ρ{βa } , Oa  } = 0 .

(2.40)

However, ρ{βa } becomes stationary with respect to each of these individual flows Xa  (in addition to always being stationary with respect to the full modular flow), if the generators of the individual flows commute with each other, that is {Oa  , Oa  } = 0 (for all a  , a  )

⇒

Xa  (ρ{βa } ) = 0 (for any a  ) .

(2.41)

See Appendix 1 for details. In the quantum case, a generalised Gibbs density operator ρˆ{βa } of the form (2.34), ˆ satisfies the KMS condition with respect to its modular flow14 ei ht (parametrized by t ∈ R) on a given Hilbert space, generated by the modular Hamiltonian operator, hˆ =



βa Oˆ a .

(2.42)

a

Then, the state is stationary with respect to the modular flow, ˆ =0 [ρˆ{βa } , h]

(2.43)

while, it is not at equilibrium with respect to the separate flows in general, [ρˆ{βa } , Oˆ a  ] = 0

(2.44)

where, [., .] denotes a commutator bracket. But as before, we have that [Oˆ a  , Oˆ a  ] = 0 (for all a  , a  )

⇒

[ρˆ{βa } , Oˆ a  ] = 0 (for any a  ) .

(2.45)

See Appendix 1 for details. Therefore, we see that generalised Gibbs states, both classical and quantum, are stationary with respect to the modular flow extracted from the state itself, as expected from statistical mechanics. But we also see that none of the individual observables

14

ˆ

Notice that  ≡ eh is the modular operator of Tomita-Takesaki theory [4, 5].

34

2 Generalised Statistical Equilibrium

are in any way preferred or special, thus giving a generalised notion of equilibrium, with all the characterising observables being on an equal footing. In the special case when the different observable generators Oa are independent of each other, then the state is additionally stationary with respect to each of the different flows generated by them. Also in this case, the individual flows commute with each other. Thus, the system retains its equilibrium properties even when it evolves along any of these directions Xa , and not only along the specific direction defined by the superposition (2.39). Finally, we remark on one aspect that seems to differentiate the quantum from the classical case discussed above. For an operational implementation of Jaynes’ procedure in a quantum system, the constraints (2.33) can exist only if the operators Oˆ a all commute with each other, that is if the observables under study are compatible. One could thus argue, that since this requirement is operationally unavoidable for a quantum system, then a quantum generalised Gibbs state will always satisfy (2.45). A more detailed understanding, overall, of fundamental differences between the quantum and classical cases (for instance, [46]) for generalised Gibbs states requires further investigation, and is left to future work.

2.2.5 Remarks In this section we make additional remarks about the thermodynamical characterisation, highlighting many of its interesting features [26]. We notice that this notion of equilibrium is inherently observer-dependent because of its use of the macrostate thermodynamic description of the system, which in itself is observer-dependent due to having to choose a coarse-graining, that is the set of macroscopic observables [47, 48]. Further, the role of information entropy is shown to be instrumental in defining (local15 ) equilibrium states.16 It is also interesting to notice that Bekenstein’s arguments [49] can be observed to be influenced by Jaynes’ information-theoretic insights surrounding entropy, and these same insights have now guided us in the issue of background independent statistical equilibrium. To be clear, the use of the most probable distributions as characterising statistical equilibrium is not new in itself. It was used by Boltzmann in the late 19th century, and utilised (also within a Boltzmann interpretation of statistical mechanics) in a constrained system in [17]. Nor is the fact that equilibrium configurations maximise the system’s entropy, which was well known already since the time of Gibbs.17 The novelty here is: in the revival of Jaynes’ information-theoretic perspective, of deriv15

Local, in the sense of being observer-dependent. As noted by Jaynes: “...thus entropy becomes the primitive concept with which we work, more fundamental even than energy...” [24]. 17 But as Jaynes points out in [24], these properties were relegated to side remarks in the past, not really considered to be fundamental to the theory, nor to the justifications for the methods of statistical mechanics. 16

2.2 Generalised Gibbs Equilibrium

35

ing equilibrium statistical mechanics in terms of evidential probabilities, solely as a problem of statistical inference without depending on the validity of any further conjectures, physical assumptions or interpretations [24, 25, 43]; and, in the suggestion that it is general enough to apply to genuinely background independent systems, including quantum gravity. Below we list some of these more valuable features. • The procedure is versatile, being applicable to a wide array of cases (both classical and quantum), technically relying only on a sufficiently well-defined mathematical description in terms of a state space, along with a set of observables with dynamically constant averages Ua defining a suitable macrostate of the system.18 • Evidently, this manner of defining equilibrium statistical mechanics (and from it, thermodynamics) does not lend any fundamental status to energy, nor does it rely on selecting a single, special (energy) observable out of the full set {Oa }. It can thus be crucial in settings where concepts of time and energy are dubious at the least, or not defined at all like in non-perturbative quantum gravity. • It has a technical advantage of not needing any (1-parameter) symmetry (sub-) groups of the system to be defined a priori, unlike the dynamical characterisation based on the KMS condition. • It is independent of additional physical assumptions, hypotheses or principles that are common to standard statistical physics, and in the present context, to the other proposals of generalised equilibrium recalled in Sect. 2.2.2. Some examples of these extra ingredients that we encountered above in Sect. 2.2.2 are ergodicity, weak interactions, statistical independence, and often a combination of them. These are not required in the thermodynamical characterisation. • It is independent of any physical interpretations attached (or not) to the observables involved. This further amplifies its appeal for use in quantum gravity where the geometrical and physical meanings of the quantities involved may not necessarily be clear from the start. • One of the main features is the generality in the choice of observables Oa allowed naturally by this characterisation. This also helps accommodate the other proposals as special cases of this one. In principle, Oa and Ua need only be mathematically well-defined in the given description of the system (regardless of whether it is kinematic i.e. working at the extended state space level, or dynamic, i.e. working with the physical state space), such that the resultant Gibbs state is normalisable. More standard choices include a Hamiltonian in a non-relativistic system, a clock Hamiltonian in a deparametrized system [14, 18, 19, 22], and generators of kinematic symmetries like rotations, or more generally of 1-parameter subgroups of Lie group actions [29, 39]. Some of the more unconventional choices include observables like volume [17, 19, 24] (Sect. 5.1.1), (component functions of the) momentum map associated with geometric closure of classical polyhedra [20, 21] (Sect. 5.1.3.1), half-link gluing (or face-sharing) constraints of discrete gravity [20] (Sect. 5.1.3.2), a projector in group field theory [20, 38], kinetic and ver18

In fact, in hindsight, we could already have anticipated a possible equilibrium description in terms of these constants, whose existence is assumed from the start.

36

2 Generalised Statistical Equilibrium

tex operators in group field theory [26] (Sect. 3.4) and generic gauge-invariant observables (not necessarily symmetry generators) [17]. For instance, (2.41) shows that the proposal of [12, 15] based on statistical independence, i.e. (2.46) [Xρ1 , Xρ2 ] = 0 can be understood as a special case of this one, when the state is characterised by a pair of observables that are defined from the start on mutually exclusive subspaces of the state space. In this case, their respective flows will automatically commute and the state will be said to satisfy statistical independence. In Sect. 5.1 we will present several examples of applying such notions of generalised equilibrium in background independent discrete quantum gravity, and take first steps towards thermal investigations of these candidate quantum gravitational degrees of freedom subsequently in Sects. 5.2 and 5.3.

2.3 Generalised Thermodynamics Traditional thermodynamics is the study of energy and entropy exchanges. But what is a suitable generalisation of it for background independent systems? This, like the question of a generalised equilibrium statistical mechanics which we have considered till now, is still open. In the following, we offer some insights gained from preceding discussions, including identifying certain thermodynamic potentials, and generalised zeroth and first laws [26].

2.3.1 Thermodynamic Potentials and Multivariable Temperature Thermodynamic potentials are vital, particularly in characterising the different phases of a system. The most important variable is the partition function Z {βa } , giving the free energy of the system ({βa }) := − ln Z {βa } .

(2.47)

It encodes complete information about the system from which other thermodynamic quantities can be derived in principle. Notice that the standard definition of a free energy F comes with an additional factor of a (single, global) temperature, that is, we ˜ = β F. But for now,  is the more suitable quantity to define and normally have  not F since we do not (yet) have a single common temperature for the full system. We will return to this point below in Sect. 2.3.2. Next is the entropy for generalised Gibbs states of the form (2.31) or (2.34), which is given by

2.3 Generalised Thermodynamics

37

S({Ua }) =



βa Ua −  .

(2.48)

a

Notice that Jaynes’ method [24, 25], which forms the basis of the thermodynamical characterisation, identifies information entropy (given in Eq. (2.29)) with the above thermodynamic entropy, since the former is the starting point of this procedure. Also, notice again the lack of a single β scaling the whole equation at this more general level of equilibrium. Further, a set of generalised heats can be defined by varying S, dS =



βa (dUa − dOa ) =:

a



βa d Q a

(2.49)

a

where, dUa are assumed to be independent variations [24]. From this (at least part of the19 ) work done on the system dWa [20, 26], can be identified dWa := dOa  =

1 βa

 dλ 

δ dOa δOa

(2.50)

where δ denotes functional derivatives. From the setup of the thermodynamical characterisation presented in Sect. 2.2.3, we can immediately identify Ua as generalised ‘energies’. Jaynes’ procedure allows these quantities to democratically play the role of generalised energies. None had to be selected as being the energy in order to define equilibrium. This a priori democratic status of the several conserved quantities can be broken most easily by preferring one over the others. In turn if its modular flow can be associated with a physical evolution parameter (relational or not), then this observable can play the role of a dynamical Hamiltonian. Thermodynamic conjugates to these energies are several generalised inverse temperatures βa . By construction each βa is the periodicity in the flow of Oa , in addition to being the Lagrange multiplier for the ath constraint in (2.27). Moreover these same constraints can determine βa , by inverting the equations

or equivalently from

∂ = Ua , ∂βa

(2.51)

∂S = βa . ∂Ua

(2.52)

By this we mean that the term d Oa , based on the same observables defining the generalised energies Ua , can be seen as reflecting some work done on the system. But naturally we do not expect or claim that this is all the work that is/can be performed on the system by external agencies. In other words, there could be other work contributions, in addition to the terms d Wa . A better understanding of work terms in this background independent setup, will also contribute to a better understanding of the generalised first law presented below.

19

38

2 Generalised Statistical Equilibrium

In general, {βa } is a multivariable inverse temperature. In the special case when Oa are component functions of a dual vector, then β ≡ (βa ) is a vector-valued temperature. For example, this is the case when O ≡ {Oa } are dual Lie algebra-valued momentum maps associated with Hamiltonian actions of Lie groups, as introduced by Souriau [29, 39], and appearing in the context of classical polyhedra in [20, 21] (see Sect. 5.1.3.1).

2.3.2 Single Common Temperature As we saw above, generalised equilibrium is characterised by several inverse temperatures, but an identification of a single common temperature for the full system is of obvious interest. This is the case [15, 20, 26] when the modular Hamiltonian h=



βa Oa

(2.53)

a

satisfies the thermodynamical characterisation via a single constraint h = constant

(2.54)

instead of several of them (2.27), resulting in a state associated with a rescaled modular Hamiltonian h˜ = βh, now characterised by a single inverse temperature β, ρ˜β =

1 −h˜ 1 −βh e = e . ˜ ˜ Zβ Zβ

(2.55)

Clearly, this case is physically distinct from the previous, more general one. Here, we have a weaker, single constraint corresponding to the situation in which there would be an exchange of information between the different observables (so that they can thermalise to a single β). This can happen for instance when one observable is special (say, the Hamiltonian) and the rest are functionally related to it (like the volume or number of particles). Whether such a determination of a single temperature can be brought about by a more physically meaningful technique is left to future work. Having said that, it will not change the general layout of the two cases, with a single β or a set of several βa , as outlined above. One immediate consequence of extracting a single β is regarding the free energy, which can now be written in the familiar form as  = βF .

(2.56)

2.3 Generalised Thermodynamics

39

This is most directly seen from the expression for the entropy, S˜ = −ln ρ˜β ρ˜β = β



βa U˜ a + ln Z˜

⇔

F˜ = U˜ − β −1 S˜

(2.57)

a

 where U˜ = a βa U˜ a is a total energy, and tildes mean that the quantities are associated with the state ρ˜β . Notice that the above equation clearly identifies a single conjugate variable to entropy, the temperature β −1 . It is important to remark that in the above method to get a single β, we still didn’t need to choose a special observable, say O , out of the given set of Oa . If one were to do this, i.e. select O as a dynamical energy (so that by extension it is a function of the other Oa ), then by standard arguments, the rest of the Lagrange multipliers will be proportional to β  , which in turn would then be the common inverse temperature for the full system. The point is that this latter instance is a special case of the former.

2.3.3 Generalised Zeroth and First Laws We end with zeroth and first laws of generalised thermodynamics. The crux of the zeroth law is a definition of equilibrium. Standard statement refers to a thermalisation resulting in a single temperature being shared by any two systems in thermal contact. This can be extended by the statement that at equilibrium, all inverse temperatures βa are equalised. This is in exact analogy with all intensive thermodynamic parameters, such as the chemical potential, being equal at equilibrium. The standard first law is basically a statement about conservation of energy. In the generalised equilibrium case corresponding to a set of individual constraints (2.27), the first law is satisfied ath-energy-wise, dUa = d Q a + dWa .

(2.58)

The fact that the law holds a-energy-wise is not surprising because the separate constraints (2.27) for each a mean that observables Oa do not exchange any information amongst themselves. If they did, then their Lagrange multipliers would no longer be mutually independent and we would automatically reduce to the special case of having a single β at equilibrium. On the other hand, for the case with a single β, variation of the entropy (2.57) gives  βa (dUa − dOa ) =: βd Q˜ (2.59) d S˜ = β a

giving a first law with a more familiar form, in terms of total energy, total heat and total work variations d U˜ = d Q˜ + d W˜ . (2.60)

40

2 Generalised Statistical Equilibrium

As before, in the even more special case where β is conjugate to a single preferred energy, then this reduces to the traditional first law. We leave the consideration of the second law for the generalised entropy to future work. We also leave a detailed study of the quantities introduced above and physical consequences of their corresponding thermodynamics to future work.

Appendix: Stationarity with Respect to Constituent Generators We show that a generalised Gibbs state is stationary with respect to each of the indiˆ if vidual, constituent generators, Oa or Oˆ a , of the full modular hamiltonian, h or h, these generators of the individual flows all commute with each other. Lemma 1 For a classical state ρ{βa } given in (2.31), we have {Oa  , Oa  } = 0 (for all a  , a  )

Xa  (ρ{βa } ) = 0 (for any a  )

⇒

(2.61)

i.e. implication in (2.41) is true. Proof 1. The line of reasoning is summarised by the following set of relations: for any a  , a  {Oa  , Oa  } = 0 ⇒ {h, Oa  } = 0 ⇔ {h , Oa  } = 0 k

⇒ {e

−h

, Oa  } = 0

which are detailed in Lemmas 1.1–1.3 below. Lemma 1.1. {Oa  , Oa  } = 0 ⇒ {h, Oa  } = 0, as in relation (2.62).

(2.62) (2.63) (2.64) 

Proof 1.1. Using Eq. (2.36) and linearity of the Poisson bracket, we have: {h, Oa  } = {



βa  Oa  , Oa  }

(2.65)

βa  {Oa  , Oa  } .

(2.66)

a 

=

 a 

Lemma 1.2. {h, Oa  } = 0 ⇔ {h k , Oa  } = 0, for k ∈ N, as in relation (2.63). Proof 1.2. By induction, we have {h k , Oa  } = kh k−1 {h, Oa  }



(2.67)

2.3 Generalised Thermodynamics

41

where we have recursively used the product rule for the Poisson bracket, and commutativity of the associative product of the Poisson algebra of smooth functions over . The implication “⇐” is true, since the equality in (2.67) holds for arbitrary non-zero k and h.  Lemma 1.3. {h k , Oa  } = 0 ⇒ {e−h , Oa  } = 0, as in relation (2.64). Proof 1.3. Using the formal exponential expansion, and linearity of the Poisson bracket, we have {e−h , Oa  } = { =

∞  (−1)k

k=0 ∞  k=0

k!

h k , Oa  }

(−1)k k {h , Oa  } . k!

(2.68)

(2.69) 

Lemma 2 For a quantum state ρˆ{βa } given in (2.34), we have [Oˆ a  , Oˆ a  ] = 0 (for all a  , a  )

[ρˆ{βa } , Oˆ a  ] = 0 (for any a  )

⇒

(2.70)

i.e. implication in (2.45) is true. Proof 2. The proof follows the following line of reasoning: for any a  , a  ˆ Oˆ a  ] = 0 [Oˆ a  , Oˆ a  ] = 0 ⇒ [h, ⇒ [h , Oˆ a  ] = 0 ˆk

⇒ [e

−hˆ

, Oˆ a  ] = 0

(2.71) (2.72) (2.73)

with details of each provided in the following Lemmas 2.1–2.3, as done previously.  ˆ Oˆ a  ] = 0, as in relation (2.71). Lemma 2.1 [Oˆ a  , Oˆ a  ] = 0 ⇒ [h, Proof 2.1. Using Eq. (2.42) and linearity of the commutator bracket, we have ˆ Oˆ a  ] = [ [h,



βa  Oˆ a  , Oˆa  ]

(2.74)

βa  [Oˆ a  , Oˆ a  ] .

(2.75)

a 

=

 a 

 ˆ Oˆ a  ] = 0 ⇒ [hˆ k , Oˆ a  ] = 0, as in relation (2.72). Lemma 2.2 [h,

42

2 Generalised Statistical Equilibrium

Proof 2.2. By induction, we have [hˆ k , Oˆ a  ] =

k−1 

ˆ Oˆ a  ]hˆ j hˆ k− j−1 [h,

(2.76)

j=0

where we have a[b, c] + [a, c]b.

recursively

used

the

commutator

identity,

[ab, c] = 

ˆ

Lemma 2.3 [hˆ k , Oˆ a  ] = 0 ⇒ [e−h , Oˆ a  ] = 0, as in relation (2.73). Proof 2.3. Using the formal exponential expansion, and linearity of the commutator bracket, we have ˆ

[e−h , Oa  ] = [ =

∞  (−1)k

k=0 ∞  k=0

k!

hˆ k , Oˆ a  ]

(−1)k ˆ k ˆ [h , Oa  ] . k!

(2.77)

(2.78) 

References 1. Kubo R (1957) Statistical mechanical theory of irreversible processes. 1. General theory and simple applications in magnetic and conduction problems. J Phys Soc Jap 12:570–586. https:// doi.org/10.1143/JPSJ.12.570 2. Martin PC, Schwinger JS (1959) Theory of many particle systems. 1. Phys Rev 115:1342–1373. https://doi.org/10.1103/PhysRev.115.1342 3. Haag R, Hugenholtz NM, Winnink M (1967) On the Equilibrium states in quantum statistical mechanics. Commun Math Phys 5:215–236. https://doi.org/10.1007/BF01646342 4. Haag R (1992) Local quantum physics: fields, particles, algebras. Texts and monographs in physics. Springer, Berlin, Germany 5. Bratteli O, Robinson DW (1997) Operator algebras and quantum statistical mechanics. Vol 2: equilibrium states, Models in quantum statistical mechanics, 2nd edn. Springer, Berlin Heidelberg 6. Anderson E (2012) Problem of time in quantum gravity. Annalen der Physik 524 (12):757–786. https://doi.org/10.1002/andp.201200147 7. Höhn PA, Smith ARH, Lock MPE (2019) The trinity of relational quantum dynamics. https:// doi.org/10.1103/PhysRevD.104.066001 8. Kiefer C (2017) Does time exist in quantum gravity? In: Lehmkuhl D, Schiemann G, Scholz E (eds) Towards a theory of spacetime theories. Springer, New York, pp 287–295. ISBN 9781-4939-3210-8. https://doi.org/10.1007/978-1-4939-3210-8_10 9. Rovelli C (2011) Forget time. Found Phys 41:1475–1490. https://doi.org/10.1007/s10701-0119561-4 10. Rovelli C (1991) Time in quantum gravity: an hypothesis. Phys Rev D 43:442–456. https:// doi.org/10.1103/PhysRevD.43.442

References

43

11. Rovelli C (1995) Analysis of the distinct meanings of the notion of ‘time’, in different physical theories. Nuovo Cim. B 110:81–94. https://doi.org/10.1007/BF02741291 12. Rovelli C (1993) Statistical mechanics of gravity and the thermodynamical origin of time. Class Quant Grav 10:1549–1566. https://doi.org/10.1088/0264-9381/10/8/015 13. Connes A, Rovelli C (1994) Von Neumann algebra automorphisms and time thermodynamics relation in general covariant quantum theories. Class Quant Grav 11:2899–2918. https://doi. org/10.1088/0264-9381/11/12/007 14. Rovelli C (2013) General relativistic statistical mechanics. Phys Rev D87(8):084055. https:// doi.org/10.1103/PhysRevD.87.084055 15. Chirco G, Haggard HM, Rovelli C (2013) Coupling and thermal equilibrium in generalcovariant systems. Phys Rev D88:084027. https://doi.org/10.1103/PhysRevD.88.084027 16. Rovelli C, Smerlak M (2011) Thermal time and the Tolman-Ehrenfest effect: temperature as the ‘speed of time’. Class Quant Grav 28:075007. https://doi.org/10.1088/0264-9381/28/7/ 075007 17. Montesinos M, Rovelli C (2001) Statistical mechanics of generally covariant quantum theories: a Boltzmann-like approach. Class Quant Grav 18:555–569. https://doi.org/10.1088/02649381/18/3/314 18. Chirco G, Josset T (2016) Statistical mechanics of covariant systems with multi-fingered time. arXiv:1606.04444 19. Kotecha I, Oriti D (2018) Statistical equilibrium in quantum gravity: Gibbs states in group field theory. New J Phys 20(7):073009. https://doi.org/10.1088/1367-2630/aacbbd 20. Chirco G, Kotecha I, Oriti D (2019) Statistical equilibrium of tetrahedra from maximum entropy principle. Phys Rev D99(8):086011. https://doi.org/10.1103/PhysRevD.99.086011 21. Chirco G, Kotecha I (2019) Generalized Gibbs ensembles in discrete quantum gravity. In: Nielsen F, Barbaresco F (eds) Geometric science of information 2019. Lecture notes in computer science (LNCS). Springer, Cham 22. Chirco G, Josset T, Rovelli C (2016) Statistical mechanics of reparametrization-invariant systems. It takes three to tango. Class Quant Grav 33(4):045005. https://doi.org/10.1088/02649381/33/4/045005 23. Haggard HM, Rovelli C (2013) Death and resurrection of the zeroth principle of thermodynamics. Phys Rev D87(8):084001. https://doi.org/10.1103/PhysRevD.87.084001 24. Jaynes ET (1957) Information theory and statistical mechanics. Phys Rev 106:620–630. https:// doi.org/10.1103/PhysRev.106.620 25. Jaynes ET (1957) Information theory and statistical mechanics. II. Phys Rev 108:171–190. https://doi.org/10.1103/PhysRev.108.171 26. Kotecha I (2019) Thermal quantum spacetime. Universe 5(8):187. https://doi.org/10.3390/ universe5080187 27. Kiefer C (2004) Quantum gravity. Int Ser Monogr Phys 124:1–308 28. Rovelli C (2004) Quantum gravity. Cambridge monographs on mathematical physics. Cambridge University Press. https://doi.org/10.1017/CBO9780511755804 29. Marle C-M (2016) From tools in symplectic and poisson geometry to J.-M. Souriau’s theories of statistical mechanics and thermodynamics. Entropy 18(10). ISSN 1099-4300. https://doi. org/10.3390/e18100370. http://www.mdpi.com/1099-4300/18/10/370 30. Rovelli C (2001) A note on the foundation of relativistic mechanics. arxiv:gr-qc/0111037 31. Henneaux M, Teitelboim C (1992) Quantization of gauge systems. ISBN 978-0-691-03769-1 32. Rovelli C (1990) Quantum mechanics without time: a model. Phys Rev D 42:2638–2646. https://doi.org/10.1103/PhysRevD.42.2638 33. Bratteli O, Robinson DW (1987) Operator algebras and quantum statistical mechanics. Vol 1: C* and W* algebras, symmetry groups, decomposition of states, 2nd edn. Springer, Berlin Heidelberg 34. de Beauregard OC, Tribus MM (1974) Information theory and thermodynamics. Helv Phys Acta 47(2) 35. Landau LD, Lifshitz EM (1980) Statistical physics, part 1, vol 5. Course of theoretical physics. Butterworth-Heinemann, Oxford. ISBN 9780750633727

44

2 Generalised Statistical Equilibrium

36. Chirco G, Laudato M, Mele FM (2021) Covariant momentum map thermodynamics for parametrized field theories. Int J Geom Meth Mod Phys 18(02):2150018. https://doi.org/10. 1142/S0219887821500183 37. Chirco G, Laudato M, Mele FM (2019) Multi-symplectic lie group thermodynamics for covariant field theories. In: Nielsen F, Barbaresco F (eds) Geometric science of information. Springer, Cham. ISBN 978-3-030-26980-7 38. Oriti D (2016) Group field theory as the 2nd quantization of loop quantum gravity. Class Quant Grav 33(8):085005. https://doi.org/10.1088/0264-9381/33/8/085005 39. Souriau J-M (1997) Structure of dynamical systems: a symplectic view of physics, vol 149. Springer Science & Business Media. https://doi.org/10.1007/978-1-4612-0281-3. Translation of Structure des Systemes Dynamiques, 1969, Dunod 40. Krasnov KV (1997) Geometrical entropy from loop quantum gravity. Phys Rev D 55:3505– 3513. https://doi.org/10.1103/PhysRevD.55.3505 41. Martinetti P, Rovelli C (2003) Diamond’s temperature: unruh effect for bounded trajectories and thermal time hypothesis. Class Quant Grav 20:4919–4932. https://doi.org/10.1088/02649381/20/22/015 42. Haggard HM (2018) Gibbsing spacetime: a group field theory approach to equilibrium in quantum gravity. New J Phys 20(7):071001. https://doi.org/10.1088/1367-2630/aad1ac 43. Jaynes ET (1979) Where do we stand on maximum entropy? In: Levine RD, Tribus M (eds) Maximum entropy formalism. MIT Press 44. Uffink J (2011) Subjective probability and statistical physics. In: Beisbart C, Hartmann S (eds) Probabilities in physics. Oxford University Press, p 25 45. Spekkens RW (2007) Evidence for the epistemic view of quantum states: a toy theory. Phys Rev A 75:032110. https://doi.org/10.1103/PhysRevA.75.032110 46. Spekkens RW (2016) Quasi-quantization: classical statistical theories with an epistemic restriction. In: Chiribella G, Spekkens RW (eds) Quantum theory: informational foundations and foils. Springer Netherlands, Dordrecht, pp 83–135. ISBN 978-94-017-7303-4. https://doi.org/ 10.1007/978-94-017-7303-4_4 47. Jaynes ET (1992) The Gibbs paradox. In: Ray Smith C, Erickson GJ, Neudorfer PO (eds) Maximum entropy and Bayesian methods. Springer Netherlands, Dordrecht, pp 1–21. ISBN 978-94-017-2219-3. https://doi.org/10.1007/978-94-017-2219-3_1 48. Jaynes ET (1965) Gibbs vs. Boltzmann entropies. Am J Phys 33(5):391–398. https://doi.org/ 10.1119/1.1971557 49. Bekenstein JD (1973) Black holes and entropy. Phys Rev D7:2333–2346. https://doi.org/10. 1103/PhysRevD.7.2333

Chapter 3

Many-Body Quantum Spacetime

The beginnings of all things are small. —Marcus Tullius Cicero

Now that we have presented a potential generalisation of statistical equilibrium in the previous chapter, we move on to its application in discrete quantum gravity. As anticipated in Sect. 1.3, in this thesis a discrete quantum spacetime is modelled as a many-body system composed of a large number of elementary building blocks,1 or quanta of space [1]. Specifically, the candidate atoms of space under consideration here are geometric convex d-polyhedra with d bounding faces, dual to open d-valent nodes with its half-links dressed by suitable algebraic data [2]. This choice is motivated strongly by loop quantum gravity (LQG) [3–5], spin foams [6, 7], group field theory [8–14], dynamical triangulations [15] and lattice quantum gravity [16] approaches in the context of 4d models. Extended discrete quantum space can be built out of these fundamental ‘atoms’ or ‘particles’, via kinematical compositions (or boundary gluings), and spacetime via dynamical interactions (or bulk bondings). The perspective innate to such a many-body quantum spacetime is thus a constructive one, which is then naturally also extended to the statistical mechanics based on this many-body mechanics. As we will see, two types of data specify a mechanical model, combinatorial and algebraic. States and processes of a model are supported on combinatorial structures, here abstract2 graphs and 2-complexes respectively; and algebraic dressings of these 1

We should emphasise that in any non-spacetime-based, background independent setting (like the present one), elementary quanta of geometry are not “small” in the conventional intuitive sense; and, “large” spacetime is not simply a sum of many “small” building blocks, in the additive sense. Rather, continuum spacetime must emerge from the collective dynamics, coarse graining and composite properties of the underlying constituents. 2 Thus not necessarily embedded into any continuum spatial manifold. © The Author(s), under exclusive license to Springer Nature Switzerland AG 2022 I. Kotecha, On Generalised Statistical Equilibrium and Discrete Quantum Gravity, Springer Theses, https://doi.org/10.1007/978-3-030-90969-7_3

45

46

3 Many-Body Quantum Spacetime

structures add discrete geometric and matter information. Thus, different choices of combinatorics and algebraic data give different mechanical models. For instance, the simplest 4d spin foam models (and their associated group field theories) are associated with: boundary combinatorics based on a 4-valent node (dual to a tetrahedron, under closure), bulk combinatorics based on a 4-simplex interaction vertex, and algebraic (or group representation) data of SU (2) labelling the boundary 4-valent graphs and bulk 2-complexes. Clearly this is not the only choice, in fact far from it. The vast richness of possible combinatorics, compatible with our constructive point of view, is comprehensively illustrated in [17]. And the various choices for variables to label the discrete structures with (so that they may encode some notion of discrete geometry, which notion depending exactly on the variables chosen and constraints imposed on them) have been an important subject of study, starting all the way from Regge [18–23]. Accommodation of these various different choices is yet another appeal of our constructive many-body viewpoint and this framework. We clarify further some of these aspects in the following, but often choose to work with simplicial combinatorics and SU (2) holonomy-flux data in the subsequent chapters. In this chapter, we use results from the previous sections to outline a framework of equilibrium statistical mechanics for these candidate quanta of geometry [24–26]. In particular, we show that a group field theory arises naturally as an effective statistical field theory from a coarse-graining of a class of generalised Gibbs configurations of the underlying quanta. In addition to providing an explicit quantum statistical basis for group field theories, this reinforces their status as being field theories for quanta of geometry [8–12]. Motivated by these discussions, we will present aspects of thermal states in group field theories in the following chapters.

3.1 Atoms of Quantum Space and Kinematics In the following we will refer to some of the combinatorial structures defined in [17]. However we will be content with introducing them in a more intuitive manner, and not recalling the rigorous definitions as that is not required for the purposes of this thesis. We refer to [17] for details.3 3

For clarity, we note that the terminology used here is slightly different from that in [17]. Specifically the dictionary between here ↔ there is: combinatorial atom or particle ↔ boundary patch; interaction/bulk vertex ↔ spin foam atom; boundary node ↔ boundary multivalent vertex v; ¯ link or full link ↔ boundary edge connecting two multivalent vertices v¯1 , v¯2 ; half-link ↔ boundary edge connecting a multivalent vertex v¯ and a bivalent vertex v. ˆ This minor difference is mainly due to a minor difference in the purpose for the same combinatorial structures. Here we are in a setup where the accessible states are boundary states, for which a statistical mechanics is defined; and the case of interacting dynamics is considered as defining a suitable (amplitude) functional over the the boundary state space. On the other hand, the perspective in [17] is more in a spin foam constructive setting, so that modelling the 2-complexes as built out of fundamental spin foam atoms is more natural there.

3.1 Atoms of Quantum Space and Kinematics

47

The primary objects of interest to us are boundary patches, which we take as the combinatorial atoms of space. To put simply, a boundary patch is the most basic unit of a boundary graph, in the sense that the set of all boundary patches generates the set of all connected bisected boundary graphs. A bisected boundary graph is simply a directed boundary graph with each of its full links bisected into a pair of halflinks, glued at the bivalent nodes (for instance, see Fig. 3.1). Different kinds of atoms of space are then the different, inequivalent boundary patches (dressed further with suitable data), and the choice of combinatorics basically boils down to a choice of the set of admissible boundary patches. Moreover, a model with multiple inequivalent boundary patches can be treated akin to a statistical system with multiple species of atoms. The most general types of boundary graphs are those with nodes of arbitrary valence, and including loops. A common and natural restriction is to consider loopless structures, as they can be associated with combinatorial polyhedral complexes [17]. As the name suggests, loopless boundary patches are those with no loops, i.e. each half-link is bounded on one end by a unique bivalent node (and on the other by the common, multivalent central node). A loopless patch is thus uniquely specified by the number of incident half-links (or equivalently, by the number of bivalent nodes bounding the central node). A d-patch, with d number of incident half-links, is simply a d-valent node. Importantly for us, it is the combinatorial atom that supports geometric states of a d-polyhedron [2, 27, 28]. A further common restriction is to consider graphs with nodes of a single, fixed valence, that is to consider d-regular loopless structures. Let’s take an example. Consider the boundary graph of a 4-simplex as shown in Fig. 3.1. The fundamental atom or boundary patch is a 4-valent node. This graph can be constructed starting from five open 4-valent nodes (denoted m, n, . . . , q), and gluing the half-links, or equivalently the faces of the dual tetrahedra, pair-wise, with the non-local combinatorics of a complete graph on five 4-valent nodes. The result is ten bisected full links, bounded by five nodes. It is important to note here that a key ingredient of constructing extended boundary states from the atoms are precisely the half-link gluing, or face-sharing conditions on the algebraic data decorating the patches. For instance, in the case of standard LQG holonomy-flux variables of T ∗ (SU (2)), the face-sharing gluing constraints are area matching [21], thus lending a notion of discrete classical twisted geometry to the graph [21, 22]. This is much weaker than a Regge geometry, which could have been obtained for the same variables if instead the so-called shape-matching conditions [20] are imposed on the pair-wise gluing of faces, or equivalently half-links. Thus, kinematic composition (boundary gluings) that creates boundary states depends on two crucial ingredients, the combinatorial structure of the resultant boundary graph, and face-sharing gluing conditions on the algebraic data. From here on we will restrict to a single boundary patch for simplicity, namely a gauge-invariant d-patch dressed with SU (2) data, dual to a d-polyhedron [2, 27]. But it should be clear from the brief discussion above (and the extensive study in [17]) that a direct generalisation of the present mechanical and statistical framework is formally possible also for these more enhanced combinatorial structures.

48

3 Many-Body Quantum Spacetime

Fig. 3.1 Bisected boundary graph of a 4-simplex, as a result of non-local pair-wise gluing of half-links. Each full link is bounded by two 4-valent nodes (shown here as rectangles), and bisected by one bivalent node (shown here as squares) [26]

The classical intrinsic geometry of a polyhedron with d faces is given by the Kapovich-Millson phase space [29], Sd = {(X I ) ∈ su(2)∗d |

d 

X I = 0, ||X I || = A I }/SU (2)

(3.1)

I =1

which is a (2d − 6)-dimensional symplectic manifold. Now, for more generality, one could lift the restriction of fixed face areas, thereby adding d degrees of freedom, to get the (3d − 6)-dimensional space of closed polyhedra, modulo rotations in R3 . For d = 4, this is the 6-dim space of a tetrahedron [27, 28], considered often in discrete quantum gravity contexts (Fig. 3.2). This space corresponds to the possible values of the 6 edge lengths of a tetrahedron, or to the 6 areas that include four areas of its faces and two independent areas of parallelograms identified by midpoints of pairs of opposite edges. This space is not symplectic in general, and to get a symplectic manifold from it, one can either remove the d area degrees of freedom to get Sd again, or add another d number of degrees of freedom, the U (1) angle conjugates to the areas, to get the spinor description of the so-called framed polyhedra [30].4 However, we are presently more interested in the statistical description of a collection of many connected, closed polyhedra. Let us then consider the space of closed polyhedra with a fixed orientation, and extend the phase space description so as to encompass the extrinsic geometric degrees of freedom, which we expect to play a role in the description of the coupling leading to a collective model. We know from above that the face normal vectors with arbitrary 4

Along the lines shown below, one can thus also extend the statistical description to the case of the framed polyhedron system.

3.1 Atoms of Quantum Space and Kinematics Fig. 3.2 a A convex polygon with a closed set of vectors X I . The space of possible polygons in R3 up to rotations is a (2d − 6)-dimensional phase space. For non-coplanar normals, the same data define also a unique polyhedron by Minkowski’s theorem. b For d = 4 we get a geometric tetrahedron. [25]

(a)

49 (b)

X4

X3

X4

X3 X1 X1 X2 X2

∼ R3 , which is a Poisson manifold areas are elements of the dual algebra su(2)∗ = with its Kirillov-Kostant Poisson structure [28]. We can supplement this data with conjugate degrees of freedom belonging to the group SU (2) (thereby also doubling the dimension) and consider the phase space, d-poly = T ∗ (SU (2)d /SU (2)) .

(3.2)

Here, the quotient by SU (2) imposes geometricclosure of the polyhedron; equivalently, it constraints the area normals to close, dI=1 X I = 0 (see also Sects. 4.1.1 and 5.1.3.1). Specifically for d = 4, we then have a single classical tetrahedron phase space given by, (3.3)  = T ∗ (SU (2)4 /SU (2)) which encodes both intrinsic and extrinsic degrees of freedom (along with an arbitrary orientation in R3 ). Notice that the choice of domain manifold is essentially the choice of algebraic data. For instance, this could be Spin(4) in Euclidean 4d settings, while S L(2, C) in Lorentzian ones. Then, the states of a system of N tetrahedra belong to the following direct product space,  N =  ×N

(3.4)

with an algebra composed of smooth real-valued functions defined on  N [24–26]. On the other hand, in a quantum setting, each closed polyhedron face I is assigned an SU (2) representation label j I with its associated representation space H jI , and the polyhedron itself with an intertwiner, i.e. an invariant tensor element of Hd-poly{ jI } = Inv

d 

H jI .

(3.5)

I =1

This is the space of d-valent intertwiners with given fixed spins { j I } i.e. given fixed face areas, corresponding to a quantisation of Sd . Then, quantisation of d-poly is the full space of d-valent intertwiners, given by

50

3 Many-Body Quantum Spacetime

Hd-poly =

 { j I ∈N/2}

Inv

d 

H jI .

(3.6)

I =1

A collection of neighbouring quantum polyhedra has been associated to a spin network of arbitrary valence [2], with the labelled nodes and links of the latter being dual to labelled polyhedra and their shared faces respectively. Then for a quantum tetrahedron [27, 28], the 1-particle Hilbert space is, H

(3.7)

with quantum states of an N -particle system belonging to the following tensor product space, (3.8) where, H0 = C. We can equivalently work with the holonomy representation of the same quantum system in terms of SU (2) group data, (3.9) which is also the state space of a single gauge-invariant quantum of a group field theory defined on an SU (2)4 base manifold (see Sect. 4.1 for details). A further, equivalent representation could be given in terms of non-commutative Lie algebra (flux) variables X I ∈ su(2)∗ [31, 32]. On such multi-particle state spaces, mechanical models for a system of many tetrahedra can be defined via constraints among them. Typical examples would be non-local, combinatorial gluing constraints, possibly scaled by an amplitude weight. From the point of view of many-body physics, we expect these gluing constraints to be modelled as generic multi-particle interactions, defined in terms of tetrahedron geometric degrees of freedom. Different choices of these interactions would then identify different models of the system. The key ingredient of such interactions are the constraints which glue two faces of any two different tetrahedra, for instance by constraining the areas of adjacent faces to match and their face normals to align (see Sect. 5.1.3.2). More stringent conditions, imposing stronger matching of geometric data, as well as more relaxed ones, can also be considered, as will be discussed. What constitutes as gluing is thus a model-building choice, and so is the choice of which combinatorial pattern of gluings among a given number of tetrahedra is enforced. So, once the system knows how to glue two faces, then the remaining content of a model dictates how the tetrahedra interact non-locally to make simplicial complexes [25, 26, 33]. More on this will be discussed in Sects. 3.2 and 5.1.3. Lastly, for a quantum multi-particle system, one can go a step further and define a Fock space to accommodate configurations with varying particle numbers. For

3.1 Atoms of Quantum Space and Kinematics

51

bosonic5 quanta, each N -particle sector is the symmetric projection of the full N particle Hilbert space, so that a Fock space can be defined as, (3.10) is degenerate with no discrete geometric The associated Fock vacuum state degrees of freedom, the ‘no space’ state. One choice for the algebra of operators is the von Neumann algebra of bounded linear operators . A more on common choice though is the larger *-algebra generated by ladder operators ϕ, ˆ ϕˆ † , by acting on the cyclic Fock vacuum, and satisfy a commutation which generate relations algebra  [ϕ( ˆ g1 ), ϕˆ ( g2 )] = †

dh SU (2)

4 

−1 δ(g1I hg2I )

(3.11)

I =1

where g ≡ (g I ) ∈ SU (2)4 and the integral on the right ensures SU (2) gauge invariance. In fact this is the Fock representation associated with a degenerate vacuum of an algebraic bosonic group field theory defined by a Weyl algebra [24, 34, 35]. We will return to a detailed discussion of these aspects in Sect. 4.1. Notice that this kind of formulation already hints at a second quantised language in terms of quantum fields of tetrahedra. This language can indeed be applied to the generalised statistical mechanics framework we have developed, to get a quantum statistical mechanics for tetrahedra (polyhedra in general), which will be the focus of the rest of the thesis.

3.2 Interacting Quantum Spacetime and Dynamics Coming now to dynamics, the key ingredients here are the specifications of propagators and admissible interaction vertices, including both their combinatorics, and functional dependences on the algebraic data i.e. their amplitudes. The combinatorics of propagators and interaction vertices can be packaged neatly within two maps, the bonding map and the bulk map respectively [17]. A bonding map is defined between two bondable boundary patches. Two patches are bondable if they have the same number of nodes and links. Then, a bonding map between two bondable patches identifies each of their nodes and links, under the compatibility condition that if a bounding bivalent node in one patch is identified with a particular one in another, then their respective half-links (attaching them to their respective central 5

As for a standard multi-particle system, bosonic statistics corresponds to a symmetry under particle exchange. For the case when a system of quantum tetrahedra is glued appropriately to form a spin network, then this symmetry is understood as implementing the graph automorphism of node relabellings.

52

3 Many-Body Quantum Spacetime

nodes) are also identified with each other. So a bonding map basically bonds two bulk vertices via (parts of) their boundary graphs to form a process (with boundary). This is simply a bulk edge, or propagator. The set of interaction vertices can themselves be defined by a bulk map. This map augments the set of constituent elements (multivalent nodes, bivalent nodes, and half-links connecting the two) of any bisected boundary graph, by one new vertex (the bulk vertex), a set of links joining each of the original boundary nodes to this vertex, and a set of two dimensional faces bounded by a triple of the bulk vertex, a multivalent boundary node and a bivalent boundary node. The resulting structure is an interaction vertex with the given boundary graph.6 The complete dynamics is then given by the chosen combinatorics, supplemented with amplitude functions that reflect the dependence on the algebraic data. The interaction vertices can in fact be described by vertex operators on the Fock space in terms of the ladder operators. An example vertex operator, corresponding to the 4-simplex boundary graph shown in Fig. 3.1, is ˆ 4sim = V

 SU (2)20

[dg] ϕˆ † ( g1 )ϕˆ † ( g2 )V4sim ( g1 , . . . , g5 )ϕ( ˆ g3 )ϕ( ˆ g4 )ϕ( ˆ g5 )

(3.12)

where the interaction kernel V4sim = V4sim ({gi j g −1 ji }i< j ) (for i, j = 1, . . . , 5) encodes the combinatorics of the boundary graph. There are of course other vertex operators associated with the same graph (that is with the same kernel), but including different combinations of creation and annihilation operators.7 It must be noted that generic configurations of this system do not admit an interpretation as quantised geometric fields. Therefore, geometric configurations cannot be presumed, and one would have to look for such phases to emerge within the full statistical description of the quanta of spacetime. This is an important and difficult open problem that we do not directly tackle in this thesis. To summarise, a definition of kinematics entails: defining the state space, which includes specifying the combinatorics (choosing the set of allowed boundary patches, which generate the admissible boundary graphs), and the algebraic data (choosing variables to characterise the discrete geometric states supported on the boundary graphs); and, defining the algebra of observables acting on the state space. A definition of dynamics entails: specifying the propagator and bulk vertex combinatorics and amplitudes. Together they specify the many-body mechanics.

6

An interesting aspect is that the bulk map is one-one, so that for every distinct bisected boundary graph, there is a unique interaction vertex which can be defined from it [17]. 7 This would generically be true for any second quantised operator [34, 36].

3.3 Generalised Equilibrium States

53

3.3 Generalised Equilibrium States Based on insights from Chap. 2 and the mechanical setup laid out above, we can formulate a statistical mechanical framework, and in particular generalised equilibrium statistical mechanics, for these discrete quantum geometric systems [24–26, 33]. For a system of many classical tetrahedra (in general, polyhedra), a statistical state ρ N can be formally defined on the state space  N . As we saw in Sect. 2.2.3, if it satisfies the thermodynamical characterisation with respect to a set of functions on  N then it will be an equilibrium state. Further, a configuration with a varying number of tetrahedra can be described by a grand-canonical type state of the form Z=



eμN Z N

(3.13)

N ≥0

 where Z N =  N dλ ρ N , and μ is a chemical potential [25]. Similarly for a system of many quantum tetrahedra, a generic statistical state ρˆ is a density operator on [24]. Generalised equilibrium states with a varying number of quanta are then given by,  ˆ ˆ (3.14) Z = Tr(e− a βa Oa +μ N )  g )ϕ( ˆ g ) is the number operator on . Such grand-canonical where Nˆ = d g ϕˆ † ( type boundary states are important because one would expect quantum gravitational dynamics to not be number conserving in general [25, 34]. Also as pointed out in Sect. 2.2.5, what the precise content of equilibrium is depends crucially on which observables Oa are used to define the state. Operators of natural interest here are the ones encoding the dynamics, that is vertex and kinetic operators, as considered below in Sect. 3.4. There are many other choices and types of observables one could consider in principle, as will be exemplified in Chap. 5. In fact, which ones are the relevant ones in a given situation is a crucial part of the whole problem. Given a density operator ρ, then the partition function Z , contains complete statistical information. From Z can be defined an important thermodynamic potential, the free energy  = − ln Z . Entropy is S = −Tr(ρ ln ρ). These thermodynamic variables are those whose construction does not really rely on the context in which the statistical mechanical framework is formulated, as we saw in Sect. 2.3. As emphasised in Chap. 2 and above, the remaining relevant macrostate variables, like generalised energies O , need to be first identified depending on the specific system at hand. Then, a macrostate of the system is characterised by this set of thermodynamic variables (and others derived from them, say via Legendre transforms), whose compatible microstates are naturally the quantum states contributing to the statistical mixture. Having done so at a formal level, naturally the remaining challenging task is to identify a suitable physical interpretation for them. For example, if a thermodynamic volume potential is defined in analogy with usual quantum field theories, this would refer to the domain manifold of the group fields, i.e. the Lie group manifold. It would not be immediately related to spatial volumes, as deduced for example by

54

3 Many-Body Quantum Spacetime

the quantum operator considered later in Sects. 5.1.1 and 5.3.1, which is motivated by the quantum geometric interpretation of the group field quanta.

3.4 Effective Statistical Group Field Theory We end this chapter by making a direct link to the definition of group field theories using the above framework. Group field theories [9–14] are non-local field theories defined over Lie groups. Most widely studied models are for real or complex scalar fields, over copies of SU (2) or Spin(4). For instance, a complex scalar GFT over SU (2) is defined by a partition function of the following general form,  Z GFT =

¯ [Dμ(ϕ, ϕ)] ¯ e−SGFT (ϕ,ϕ)

(3.15)

where μ is a functional measure which in general is ill-defined, and SGFT is the GFT action of the form, 

 SGFT =

G

dg1



 G

dg2 K (g1 , g2 )ϕ(g ¯ 1 )ϕ(g2 ) +

G

dg1

G

dg2 . . . V (g1 , g2 , . . .) f (ϕ, ϕ) ¯

(3.16)

where g ∈ G, and the kernel V is generically non-local, which convolutes the arguments of several ϕ and ϕ¯ fields (written here in terms of a single function f ). It defines the interaction vertex of the dynamics by enforcing the combinatorics of its corresponding (unique, via the inverse of the bulk map) boundary graph. Z GFT defines the covariant dynamics of a group field theory model encoded in SGFT . In this section we show a way to derive such covariant dynamics from a suitable quantum statistical equilibrium description of a system of quanta of space defined in the previous sections [26]. The following technique of using field coherent states is the same as used in [25, 34], but with the crucial difference that here we do not claim to define, or aim to achieve any correspondence (even if formal) between a canonical dynamics (in terms of a projector operator, related further to loop quantum gravity [34]) and a covariant dynamics (in terms of a functional integral). Instead we show a quantum statistical basis for the covariant dynamics itself, and in the process, reinterpret the standard form of the GFT partition function (3.15) as that of an effective statistical field theory arising from a coarse-graining, and further approximations, of the underlying statistical quantum gravity system. We discussed in Sect. 3.2 that the dynamics of the polyhedral atoms of space is encoded in the choices of propagators and interaction vertices, which can be written in terms of kinetic and vertex operators in the Fock description. In our present considerations with a single type of atom, namely SU (2)-labelled 4-valent node, let us consider the following generic kinetic and vertex operators,

3.4 Effective Statistical Group Field Theory ˆ = K ˆ = V

55

 

SU (2)8

[dg] ϕˆ † ( g1 )K ( g1 , g2 )ϕ( ˆ g2 )

SU (2)4N

[dg] Vγ ( g1 , . . . , gN ) fˆ(ϕ, ˆ ϕˆ † )

(3.17) (3.18)

where N > 2 is the number of 4-valent nodes in the boundary graph γ , and fˆ is a function of the ladder operators with all terms of a single degree N . For example when N = 3, this function could be fˆ = λ1 ϕˆ ϕˆ ϕˆ † + λ2 ϕˆ † ϕˆ ϕˆ † . As we saw before, in principle a generic model can include several distinct vertex operators. Even though ˆ the following what we consider here is the simple of case of having only one V, treatment can be extended to the general case. ˆ and V ˆ have well-defined actions on the Fock space . Using the Operators K ˆ = thermodynamical characterisation, we can consider the formal constraints8 K

ˆ , constant and V = constant, to write down a generalised Gibbs state on ρˆ{βa } =

1 Z {βa }

ˆ

ˆ

e−β1 K−β2 V

(3.19)

where a = 1, 2 and the partition function is, ˆ

ˆ

Z {βa } = Tr(e−β1 K−β2 V ) .

(3.20)

An effective field theory can then be extracted from the above by using a basis of coherent states on F [25, 26, 34, 37]. Field coherent states give a continuous representation on where the parameter labelling each state is a wavefunction [37]. For the Fock description outlined in Sect. 3.1 (and detailed in the upcoming Sect. 4.1), the Fock vacuum is specified by (3.21) The field coherent states are, (3.22)  , ||.|| is the L 2 norm in , and ϕ(ψ) ˆ = d g ψ¯ ϕˆ along with its adjoint where are the smeared ladder operators. The set of all such states provides an over-complete A very useful property of these states is that they are eigenstates of the basis for annihilation operator, ϕ( ˆ g ) |ψ = ψ( g ) |ψ . (3.23) ˆ ϕ, This property implies that, for an operator Q( ˆ ϕˆ † ) as a function of the ladder operators, we have [37], 8

A proper interpretation of these constraints is left to future work.

56

3 Many-Body Quantum Spacetime

ˆ ϕ, ¯ ψ| : Q( ˆ ϕˆ † ) : |ψ = Q(ψ, ψ)

(3.24)

where, : . : denotes normal ordering, i.e. ordering in which all ϕˆ † ’s are to the left of ¯ as the operator all annihilation operators ϕ’s, ˆ and Q is the same function of ψ and ψ, Qˆ is of ϕˆ and ϕˆ † respectively. The traces for the partition function and other observable averages can then be evaluated in this basis,  ˆ ˆ ˆ ˆ ˆ 2V ˆ ¯ ψ| e−β1 K−β = [Dμ(ψ, ψ)] O |ψ

(3.25) Tr(e−β1 K−β2 V O) ˆ

ˆ

with Z {βa } = Tr(e−β1 K−β2 V I )

(3.26)

where the resolution of identity and the coherent state functional measure are respectively given by [37], 

¯ |ψ ψ| , [Dμ(ψ, ψ)]

(3.27)

K  d Reψk d Imψk . K →∞ π k=1

(3.28)

I =

¯ = lim Dμ(ψ, ψ)

The set of all such observable averages formally defines the complete statistical system. In particular, the quantum statistical partition function can be reinterpreted as the partition function for a field theory (of complex-valued square-integrable fields) of the underlying quanta, which here are quantum tetrahedra, as follows [25, 26, 34]. ˆ ˆ ϕ, ˆ ϕˆ † ). For simplicity, let us first consider, e−β C , associated with an operator C( ˆ ˆ Then, given C and O as polynomial functions of the generators, with a given (but generic) choice of the operator ordering defining the exponential operator, the integrand of the statistical averages can be treated as follows: ˆ ψ| e−β C Oˆ |ψ = ψ|

∞  (−β)k k=0

k!

Cˆ k Oˆ |ψ

ˆ = ψ| : e−β C Oˆ : |ψ + ψ| : poC,O (ϕ, ˆ ϕˆ † , β) : |ψ

(3.29) (3.30)

where to get the second equality, we have used the commutation relations (3.11) on ˆ to collect all normal ordered terms : Cˆ k Oˆ : giving the normal ordered each Cˆ k O, −β Cˆ ˆ :e O :, and the second term is a collection of the remaining terms arising as a result of swapping ϕ’s ˆ and ϕˆ † ’s, which will then in general be a normal ordered series in powers of ϕˆ and ϕˆ † , with coefficient functions of β. The precise form of this series ˆ hence the subscripts. Using Eqs. (3.23) and (3.24), we will depend on both Cˆ and O, have: ˆ ¯ ¯ ψ| : e−β C Oˆ : |ψ = e−βC[ψ,ψ] O[ψ, ψ] (3.31)

3.4 Effective Statistical Group Field Theory

57

¯ = ψ| : Cˆ : |ψ and O[ψ, ψ] ¯ = ψ| : Oˆ : |ψ ; and, where C[ψ, ψ] ¯ β] . ψ| : poC,O (ϕ, ˆ ϕˆ † , β) : |ψ ≡ ψ| : Aˆ C,O (ϕ, ˆ ϕˆ † , β) : |ψ = AC,O [ψ, ψ, (3.32) Thus, averages can be written as ˆ

ˆ = Tr(e−β C O)





¯ ¯ ¯ + AC,O [ψ, ψ, ¯ β] . [Dμ(ψ, ψ)] e−βC[ψ,ψ] O[ψ, ψ]

(3.33)

In particular, the quantum statistical partition function is  Z=



¯ ¯ ¯ β] =: Z 0 + Z O() [Dμ(ψ, ψ)] e−βC[ψ,ψ] + AC,I [ψ, ψ,

(3.34)

where, by notation O() we mean only that this sector of the full theory encodes all higher orders in quantum terms relative to Z 0 .9 This full set of observable averages (or correlation functions) (3.33), including the above partition function, defines thus a statistical field theory of quantum tetrahedra (or in general, polyhedra with a fixed number of boundary faces), characterised by a combinatorially non-local statistical weight, that is, a group field theory. If we are further able to either reformulate exactly, or under suitable approximations, AC,O in the following way, ¯ β] O[ψ, ψ] ¯ AC,O = AC,I [ψ, ψ,

(3.35)

then, the partition function (3.34) defines a statistical field theory for the algebra of ¯ for a dynamical system of complex-valued square-integrable observables O[ψ, ψ], fields ψ, defined on the base manifold SU (2)4 . The integrands in (3.25) and (3.26) can then be treated and simplified along the lines above, in particular to get an effective partition function,  Zo =

¯ e−β1 K [Dμ(ψ, ψ)]

¯ ¯ [ψ,ψ]−β 2 V [ψ,ψ]

= Z {βa } − Z O()

(3.36)

where subscript o indicates that we have neglected higher order terms, collected inside Z O() , resulting from normal orderings of the exponent in Z {βa } . As before, ˆ : |ψ and V = ψ| : V ˆ : |ψ . It is the functions in the exponent are K = ψ| : K then evident that Z o has the precise form of a generic GFT partition function of the form (3.15). It thus defines a group field theory as an effective statistical field theory, that is (3.37) Z GFT := Z o .

9

Further investigation into the interpretation, significance and consequences of this rewriting of Z in discrete quantum gravity is left for future work.

58

3 Many-Body Quantum Spacetime

From this perspective, it is clear that the generalised inverse temperatures (which are basically the intensive parameters conjugate to the generalised energies in the generalised thermodynamical setting of Sect. 2.3) are the coupling parameters defining the effective model, thus characterising the phases of the emergent statistical field theory, as would be expected. Moreover, from this purely statistical standpoint, we can understand the GFT action more appropriately as Landau-Ginzburg free energy (or effective ‘Hamiltonian’, in the sense that it encodes the effective dynamics), instead of a Euclidean action which might imply having Wick rotated a Lorentzian measure, even in an absence of any such notions as is the case presently. Lastly, deriving like this the covariant definition of a group field theory, based entirely on the framework presented here, strengthens the statement that a group field theory is a field theory of combinatorial and algebraic quanta of space [11, 12].

References 1. Oriti D (2018) Spacetime as a quantum many-body system. In: Angilella GGN, Amovilli C (eds) Many-body approaches at different scales: a tribute to Norman H. March on the occasion of his 90th birthday. Springer International Publishing, Cham, pp 365–379. ISBN 978-3-31972374-7. https://doi.org/10.1007/978-3-319-72374-7_29 2. Bianchi, E, Dona P, Speziale S (2011) Polyhedra in loop quantum gravity. Phys Rev D 83:044035. https://doi.org/10.1103/PhysRevD.83.044035 3. Ashtekar A, Lewandowski J (2004) Background independent quantum gravity: a status report. Class Quant Grav 21:R53. https://doi.org/10.1088/0264-9381/21/15/R01 4. Rovelli C (2004) Quantum gravity. Cambridge monographs on mathematical physics. Cambridge University Press. https://doi.org/10.1017/CBO9780511755804 5. Bodendorfer N (2016) An elementary introduction to loop quantum gravity. arXiv:1607.05129 6. Perez A (2013) The spin foam approach to quantum gravity. Living Rev Rel 16:3. https://doi. org/10.12942/lrr-2013-3 7. Rovelli C, Vidotto F (2014) Covariant loop quantum gravity: an elementary introduction to quantum gravity and spinfoam theory. Cambridge University Press. https://doi.org/10.1017/ CBO9781107706910 8. Reisenberger MP, Rovelli C (2001) Space-time as a Feynman diagram: the connection formulation. Class Quant Grav 18:121–140. https://doi.org/10.1088/0264-9381/18/1/308 9. Freidel L (2005) Group field theory: an overview. Int J Theor Phys 44:1769–1783. https://doi. org/10.1007/s10773-005-8894-1 10. Oriti D (2007) Quantum gravity as a quantum field theory of simplicial geometry. In: Fauser B, Tolksdorf J, Zeidler E (eds) Quantum gravity: mathematical models and experimental bounds. Birkäuser, pp 101–126 11. Oriti D (2009) The group field theory approach to quantum gravity. In: Oriti D (ed) Approaches to quantum gravity: toward a new understanding of space, time and matter. Cambridge University Press 12. Oriti D (2011) The microscopic dynamics of quantum space as a group field theory. In: Proceedings, foundations of space and time: reflections on quantum gravity: Cape Town, South Africa, pp 257–320 13. Krajewski T (2011) Group field theories. PoS QGQGS2011(005). https://doi.org/10.22323/1. 140.0005 14. Gielen S (2021) Frozen formalism and canonical quantization in group field theory. https:// doi.org/10.1103/PhysRevD.104.106011

References

59

15. Loll R (2019) Quantum gravity from causal dynamical triangulations: a review. Class Quant Grav 37(1):013002. https://doi.org/10.1088/1361-6382/ab57c7 16. Hamber HW (2009) Quantum gravity on the lattice. Gen Rel Grav 41:817–876. https://doi. org/10.1007/s10714-009-0769-y 17. Oriti D, Ryan JP, Thuerigen J (2015) Group field theories for all loop quantum gravity. New J Phys 17(2):023042. https://doi.org/10.1088/1367-2630/17/2/023042 18. Regge T (1961) General relativity without coordinates. Nuovo Cim 19:558–571. https://doi. org/10.1007/BF02733251 19. Regge T, Williams RM (2000) Discrete structures in gravity. J Math Phys 41:3964–3984. https://doi.org/10.1063/1.533333 20. Dittrich B, Speziale S (2008) Area-angle variables for general relativity. New J Phys 10:083006. https://doi.org/10.1088/1367-2630/10/8/083006 21. Freidel L, Speziale S (2010) Twisted geometries: A geometric parametrisation of SU(2) phase space. Phys Rev D 82:084040. https://doi.org/10.1103/PhysRevD.82.084040 22. Rovelli C, Speziale S (2010) On the geometry of loop quantum gravity on a graph. Phys Rev D 82:044018. https://doi.org/10.1103/PhysRevD.82.044018 23. Dittrich B, Ryan JP (2011) Phase space descriptions for simplicial 4d geometries. Class Quant Grav 28:065006. https://doi.org/10.1088/0264-9381/28/6/065006 24. Kotecha I, Oriti D (2018) Statistical equilibrium in quantum gravity: Gibbs states in group field theory. New J Phys. 20(7):073009. https://doi.org/10.1088/1367-2630/aacbbd 25. Chirco G, Kotecha I, Oriti D (2019) Statistical equilibrium of tetrahedra from maximum entropy principle. Phys Rev D 99(8):086011. https://doi.org/10.1103/PhysRevD.99.086011 26. Kotecha I (2019) Thermal quantum spacetime. Universe 5(8):187. https://doi.org/10.3390/ universe5080187 27. Barbieri A (1998) Quantum tetrahedra and simplicial spin networks. Nucl Phys B 518:714–728. https://doi.org/10.1016/S0550-3213(98)00093-5 28. Baez JC, Barrett JW (1999) The quantum tetrahedron in three-dimensions and four-dimensions. Adv Theor Math Phys 3:815–850. https://doi.org/10.4310/ATMP.1999.v3.n4.a3 29. Kapovich M, Millson JJ (1996) The symplectic geometry of polygons in euclidean space. J Differ Geom 44(3):479–513. https://doi.org/10.4310/jdg/1214459218 30. Livine ER (2013) Deformations of polyhedra and polygons by the unitary group. J Math Phys 54:123504. https://doi.org/10.1063/1.4840635 31. Baratin A, Oriti D (2010) Group field theory with non-commutative metric variables. Phys Rev Lett 105:221302. https://doi.org/10.1103/PhysRevLett.105.221302 32. Baratin A, Dittrich B, Oriti D, Tambornino J (2011) Non-commutative flux representation for loop quantum gravity. Class Quant Grav 28:175011. https://doi.org/10.1088/0264-9381/28/ 17/175011 33. Chirco G, Kotecha I (2019) Generalized Gibbs ensembles in discrete quantum gravity. In: Nielsen F, Barbaresco F (eds) Geometric science of information 2019. Lecture Notes in Computer Science (LNCS). Springer, Cham 34. Oriti D (2016) Group field theory as the 2nd quantization of loop quantum gravity. Class Quant Grav 33(8):085005. https://doi.org/10.1088/0264-9381/33/8/085005 35. Kegeles A, Oriti D, Tomlin C (2018) Inequivalent coherent state representations in group field theory. Class Quant Grav 35(12):125011. https://doi.org/10.1088/1361-6382/aac39f 36. Fetter AL, Walecka JD (1971) Quantum theory of many-particle systems. International series in pure and applied physics. McGraw-Hill. https://books.google.de/books? id=Y1HwAAAAMAAJ 37. Klauder J, Skagerstam B (1985) Coherent states. World scientific. https://doi.org/10.1142/0096

Chapter 4

Group Field Theory

If the space void of all bodies, is not altogether empty; what is it then full of? Is it full of extended spirits perhaps, or immaterial substances, capable of extending and contracting themselves; which move therein, and penetrate each other without any inconveniency, as the shadows of two bodies penetrate one another upon the surface of the wall? —Gottfried W. Leibniz1

We have discussed, in the previous chapter, how group field theories can arise effectively from a coarse graining of the underlying quantum statistical system. We now turn to GFTs proper, and introduce the structures that are relevant for our subsequent applications. Group field theories are field theories of combinatorial and algebraic quanta of geometry, formally defined by a statistical partition function  Z GFT =

[Dϕκ ] e−SGFT ({ϕκ })

(4.1)

for a set of group fields {ϕκ }. They are strictly related to various other approaches like loop quantum gravity [2–4], spin foams [5, 6], causal dynamical triangulations [7], tensor models [8] and lattice quantum gravity [9]. Like in usual field theories, the kinematics is specified by a choice of the fields ϕκ , each defined in general over a domain space of direct products of Lie groups, and taking values in some target vector space. The dynamics is specified by propagators and interaction vertices encoded in a function SGFT , which can be understood as a Landau-Ginzburg free energy function in the present statistical context [10]; or as a Euclidean action from the 1

As cited in [1], p. 161.

© The Author(s), under exclusive license to Springer Nature Switzerland AG 2022 I. Kotecha, On Generalised Statistical Equilibrium and Discrete Quantum Gravity, Springer Theses, https://doi.org/10.1007/978-3-030-90969-7_4

61

62

4 Group Field Theory

point of view of standard quantum field theories [11–15]. However unlike in usual field theories, SGFT is non-local in general with respect to the base manifold. This non-locality is essential, and encodes the non-trivial combinatorial nature of the fundamental degrees of freedom and their dynamics. Moreover, the base manifold is not spacetime, but carries algebraic information associated with discrete geometric and matter degrees of freedom. Such a complete absence of any continuum spacetime structures a priori is a manifestation of background independence in group field theory, like in various other non-perturbative approaches to quantum gravity. The partition function Z GFT perturbatively generates Feynman diagrams that are labelled 2-complexes (dual to labelled stranded diagrams), with boundary states given by labelled graphs [11–15]. For the choice of models closer to loop quantum gravity and spin foam setups, the boundary states are abstract spin networks (but organised in a second quantised Hilbert space, that of a field theory [16]) and bulk processes are spin foams, both of which in turn are dual to polyhedral complexes when restricting to loopless combinatorics [17, 18]. Thus, a group field theory generates discrete quantum spacetimes made of fundamental polyhedral quanta.2 We can describe the same structures from a many-body perspective [19], and treat as more fundamental an interacting system of many such quanta. This viewpoint enables us to import formal techniques from standard many-body physics for macroscopic systems, by treating a quantum polyhedron or an open spin network node as a single particle of interest. In fact, it has allowed for tangible explorations of connections of group field theory with quantum information theory and holography [20–25], and also with quantum statistical mechanics and thermal physics [10, 26–30]. It has further allowed for importing ideas and tools from condensed matter theory, which has been crucial for instance in the development of GFT condensate cosmology [31–34]. This same perspective further leads to a modelling of an extended region of discrete quantum space (a labelled graph) as a multi-particle state, and a region of dynamical quantum spacetime (a labelled 2-complex) as an interaction process. As we have emphasised before, this is the perspective that we employ throughout the thesis to use techniques from many-body physics and statistical mechanics, even when working with a radically different kind of system, one that is background independent, and devoid of any standard notion of space, time and other associated geometric structures and standard matter couplings. The simplest class of models are scalar theories, with fields ϕ : G d → C, defined on a direct product of d copies of the local gauge group of gravity. This is the Lorentz group S L(2, C) in 4d or its Euclidean counterpart Spin(4). SU (2) is often used as the relevant subgroup in the context of quantum gravity, especially for models connected to LQG. In this thesis, G is taken to be locally compact so that the Haar measure is defined (even though it would be finite only for compact groups); connected (for 2

As discussed previously in Chap. 3, a quantised polyhedron with d faces is dual to a gauge-invariant open d-valent spin network node [17]. The latter is in fact a special case (namely, a d-patch [18]) of richer combinatorial boundary structures which can be treated analogously in our present setup, but in that case without related discrete geometric understanding of the same.

4 Group Field Theory

63

constructions in Sect. 5.1.2.1); and, unimodular so that the left- and right-invariant Haar measures coincide. These properties are satisfied by SU (2), R, Spin(4) and S L(2, C), of which the first two are used in some specific examples later in the thesis. Further, we may be interested in group field theories which generate discrete spacetimes coupled to discretised real scalar matter fields. One way to couple a single real scalar degree of freedom is by extending the original configuration space G d , encoding purely geometric data, by R. By extension, n number of scalar fields can be coupled by considering the base manifold G d × Rn [31–38]. Doing this we have assigned additional n real numbers representing the values of the fields, to each quantum of the group field. Consequently, a GFT Feynman diagram (labelled 2-complex) is enriched by n scalar fields that are discretised on the vertices of the boundary graphs (equivalently, edges of the bulk 2-complex). Thus we are concerned with a group field,  → ϕ(  g , φ) g , φ) (4.2) ϕ : G d × Rn → C, ( defined for arbitrary natural numbers n ≥ 0 and d > 0 (before any physical restrictions coming from considerations in discrete quantum gravity). The main reasons for including matter in GFTs are natural. Any fundamental theory of gravity must include, or must be able to generate at an effective level, matter degrees of freedom if it is to eventually realistically describe the universe. Also, material reference frames can be used to define physical relational observables in background independent systems [39–46]. For instance in GFT, relational reference frames defined by scalar fields have been used in the context of cosmology [31–36, 38, 47–49]. In this thesis, we make use of relational frames in two different contexts.  In Sect. 5.1.2, we define Gibbs states first with respect to internal translations in φ, and then with respect to a clock Hamiltonian associated with one of these φ’s, now being an external clock to the system after deparametrization as described in Sect. 4.2 below. Later in Sect. 5.3, we first clarify the notion of relational frames in GFT by using smearing functions along the φ direction, and then apply them in the context of thermal condensate cosmology in GFT. In this chapter, we present a quantum operator formulation of bosonic group field theories, detailing those aspects which are relevant for our later constructions. In Sect. 4.1.1, we give a Fock space construction based on the degenerate vacuum (which we also encountered in the previous chapter). In Sect. 4.1.2 we present three orthonormal bases that will be useful for later investigations. Then in Sect. 4.1.3, we give the Weyl algebraic formulation of the same system, along with the construction of their translation *-automorphisms in 4.1.4. Finally in Sect. 4.2, we consider the issue of deparametrization in group field theory based on insights and tools from presymplectic mechanics of multi-particle systems.

64

4 Group Field Theory

4.1 Bosonic Group Field Theory 4.1.1 Degenerate Vacuum and Fock Representation  can Adopting a second quantisation scheme [50–52], states of a group field ϕ( g , φ) be organised in a Fock space H F generated by a Fock vacuum | F  and the ladder operators3 {ϕ, ϕ † } [16, 53]. The vacuum is specified by  | F  = 0 , ∀ g, φ . ϕ( g , φ)

(4.3)

This is a degenerate vacuum, with no quantum geometrical or matter degrees of freedom. It is a state like 0 , the ‘no-space’ state, which we encountered previously in Sect. 3.1. We also remark that later in Sect. 5.2, a degenerate vacuum of this kind is denoted by |0, in order to declutter the overall notation of the investigation there. A single quantum is created by acting on | F  with the creation operator,    | F  = g, φ ϕ † ( g , φ)

(4.4)

which is the state of a d-valent node whose links are labelled by group elements g = (g1 , . . . , gd ) and the node itself by a set of real numbers φ = (φ1 , . . . , φn ). Then, a generic single-particle state with wavefunction ψ is given by,  |ψ =

 Gd

d g

Rn

    g , φ d φ ψ( g , φ)

(4.5)

where ψ is an element of the single-particle Hilbert space. This Hilbert space is given by4 H = L 2 (G d × Rn ) (4.6) or, when the geometric condition of closure is satisfied, by5 H = L 2 (G d /G × Rn ) ∼ = L 2 (G d /G) ⊗ L 2 (Rn ) .

3

(4.7)

Throughout the thesis, we may choose to neglect or reinstate the hat notation for operators without notice, in order to simplify or clarify the notation in the setup at hand. 4 Notice that even for compact G, the base manifold is non-compact along R, which might then demand appropriate regularisation schemes depending on the case at hand e.g. operator (5.34) in Sect. 5.1.2.1. 5 We have chosen to denote both these Hilbert spaces by the same H, because our technical results are independent of which one we choose. What changes is the interpretation of a single quantum of the group field, which can be understood as a convex polyhedron only with the latter choice.

4.1 Bosonic Group Field Theory

65

Closure corresponds to the field ϕ being invariant under a diagonal right6 action of G on G d , that is (4.8) ϕ(g I , φ) = ϕ(g I h, φ) , ∀ h ∈ G and allows for understanding the quanta of the field as convex polyhedra (in turn dual to gauge-invariant spin network nodes) [17, 57, 58]. This invariance effectively reduces the geometric part of the domain space to G d /G, as evident in the expression for H above. In this thesis however, even when imposing closure, we will continue to use a redundant parametrization for convenience and consider the gauge-invariant functions to be defined on full G d while explicitly satisfying equation (4.8). Further, we choose to impose a symmetry under arbitrary particle exchanges on the states, that is bosonic statistics. In the spin network picture, this condition reflects the graph automorphism of vertex relabelling and is a natural feature to require. For the case at hand then, the Hilbert space for bosonic quanta is the Fock space HF =



sym H⊗N

(4.9)

N ≥0

where H⊗N describes the N -particle sector, with H0 = C, and sym refers to the symmetric projection of it. This is the space that we encountered before in Sect. 3.1. We stress again that this Fock space contains arbitrary spin network excitations [16], thus the quantum gravity structures are shared with loop quantum gravity even if organised in a different way. This means that defining proper statistical equilibrium states on this Fock space truly means defining non-perturbative statistical equilibrium states in a fully background independent context and within a fundamental theory of quantum gravity based on spin network states. The ladder operators that take us between the different multi-particle sectors satisfy the commutation relations algebra,  ϕ † ( g  , φ )] = I( g , g )δ(φ − φ ) [ϕ( g , φ),  ϕ † (  ϕ( g , φ), g  , φ )] = 0 [ϕ( g , φ), g  , φ )] = [ϕ † (

(4.10) (4.11)

where, I and δ are delta distributions for functions on G d and Rn respectively. The delta distribution on G d for right gauge-invariant functions takes the form, 



I( g , g ) =

dh G

6

d 

δ(g I hg −1 I ).

(4.12)

I =1

The right gauge invariance is imposed in order to avail a quantum geometric interpretation of the quanta of the GFT field, as discussed before. An additional left gauge invariance can also be imposed, as has been done in studies in the context of homogeneous cosmologies in group field theory [31, 36, 47, 54–56]. However, our entire setup, along with the technical results based on it, will mathematically follow through with or without (either or even both) these additional symmetries and their associated geometric interpretations.

66

4 Group Field Theory

The second quantised operators (see [16] for more details in the context of LQG) are elements of the unital *-algebra generated by {ϕ, ϕ † , I }, where I is the identity operator on H F , and the adjoint † is the * operation. These elements are in general polynomials O(ϕ, ϕ † , I ) of the three. We denote this algebra by A F , with action on HF .

4.1.2 Useful Bases Spin-Momentum For compact G, by Peter-Weyl theorem, the Hilbert space L 2 (G) can be decomposed into a sum of finite-dimensional irreducible representations of G [59, 60]. Then for G = SU (2), a useful basis in L 2 (SU (2)d ) is given by the Wigner modes Dχ , labelled by a set of irreducible representation indices χ . Particularly, for right gauge-invariant functions on SU (2)d (satisfying (4.8)), this is given by the following set of Wigner functions d  j  j g) = Cm  ι DmI I m  (g I ) (4.13) Dχ ( m 

I =1

I

where χ ≡ ( j, m,  ι), j I ∈ N/2 are spin irreducible representation indices of SU (2), j m I , m I ∈ (− j I , . . . , + j I ) are matrix indices in representation j I , DmI I m  are complexI  √ valued Wigner matrix coefficients (multiplied by a factor of dim jI = 2 j I + 1, for j

normalisation shown in (4.14) below) in representation j I , and Cm  ι are intertwiner basis elements indexed by ι arising due to the closure condition in (4.8) for SU (2). Orthonormality and completeness are respectively given by,  g )Dχ  ( g ) = δχ χ  , d g Dχ (  Dχ ( g )Dχ ( g  ) = I( g , g ) .

(4.14) (4.15)

χ

While for the coupled matter degrees of freedom in L 2 (Rn ), one can consider the standard Fourier basis,  = e−i p.φ . (4.16) F( p, φ)  g , φ), The corresponding basis in H is then of the tensor product form, (Dχ ⊗ F( p))( and the algebra generators are given by the appropriate smearing,

4.1 Bosonic Group Field Theory

67

 ϕχ ( p) := ϕ(Dχ ⊗ F( p)) =



 g , φ)  , d gd φ Dχ ( g )F( p, φ)ϕ(

(4.17)

 † (  . d gd φ Dχ ( g )F( p, φ)ϕ g , φ)

(4.18)

ϕχ† ( p) = ϕ † (Dχ ⊗ F( p)) =

The algebra structure in (4.10) is preserved, and now takes the form [ϕχ ( p), ϕχ†  ( p )] = (2π )n δχ χ  δ( p − p ) 

[ϕχ ( p), ϕχ  ( p )] =

[ϕχ† ( p), ϕχ†  ( p )]

=0

(4.19) (4.20)

where δχ χ  is the Kronecker delta, and δ( p − p ) is a Dirac delta distribution on Rn . The Fock space H F is then generated via actions of {ϕχ ( p), ϕχ† ( p), I } on the vacuum | F . Discrete Index We retain the use of the Wigner basis mentioned above, labelled by discrete indices χ .  For the matter part, let us consider a basis of complex-valued smooth functions Tα (φ) in L 2 (Rn ), labelled by a set of discrete indices α = (α1 , . . . , αn ) ∈ Nn , satisfying orthonormality and completeness, 

 α  (φ)  = δα α  , d φ Tα (φ)T   α (φ ) = δ(φ − φ ) . Tα (φ)T

(4.21) (4.22)

α

We thus have a complete orthonormal basis on H consisting of functions (Dχ ⊗  of the tensor product form. Then as before, the set of mode ladder operators Tα )( g , φ) can be defined by smearing the operators ϕ, ϕ † with this basis,  aχ α := ϕ(Dχ ⊗ Tα ) =



aχ† α = ϕ † (Dχ ⊗ Tα ) =

 g , φ)  , d gd φ Dχ ( g )Tα (φ)ϕ(

(4.23)

 † ( d gd φ Dχ ( g )Tα (φ)ϕ g , φ) .

(4.24)

This essentially decomposes the operators ϕ, ϕ † in terms of the modes Dχ ⊗ Tα , which can be seen directly by inverting the above two equations. The algebra relations are, [aχ α , aχ†  α  ] = δχ χ  δα α  [aχ α , aχ  α  ] =

[aχ† α , aχ†  α  ]

(4.25) = 0.

(4.26)

 α in L 2 (Rn ), the algebra We note that due to the choice of a discrete basis {Tα (φ)} commutator in (4.25) now produces Kronecker deltas, instead of the Dirac delta

68

4 Group Field Theory

distribution of the original basis in Eq. (4.10), or the momentum basis in Eq. (4.19). The consideration of a regular algebra instead of a distributional one, particularly for the φ-modes, is an important feature in certain parts of this thesis where we deal with inequivalent representations obtained via thermal Bogoliubov transformations. Namely, the Kronecker delta δαα is crucial in order to avoid divergences related to the coincidence limit φ → φ  of δ(φ − φ  ). As we will see in Sects. 5.2.4 and 5.3.1, such terms with δ(φ − φ  ) arise naturally when calculating thermal expectation values of certain relevant observables, for example the average thermal number density. The degenerate vacuum is again specified by, aχ α | F  = 0 , ∀χ , α

(4.27)

which generates the symmetric Fock space H F by the action of the generators {aχ α , aχ† α , I }. For instance, a single particle (N = 1), single mode state is,  |χ,  α  ≡ Dχ ⊗ Tα = aχ† α | F  while a single particle state with wavefunction ψ( g , φ) = H is,

|ψ = a † (ψ) | F  =



(4.28)

χ,  α

Dχ ⊗ Tα ( g , φ)ψχ α ∈

ψχ α aχ† α | F  .

(4.29)

χ,  α

Occupation Number A good basis to work with in the Fock space is the orthonormal occupation number basis. It is particularly useful because it is the eigenbasis of the number operator, and therefore of all extensive operators, in H F . This basis organises the states according to the number of particles occupying a given mode (χ,  α ). Utilising the commutation algebra relations (4.25), a normalised multi-particle  α ) is given by, state with n χ α number of particles in a single mode (χ,  n χ α :=  1 (a † )n χ α | F  . n χ α ! χ α

(4.30)

Then, generic multi-particle states occupying several modes χi , α i are given by,  †   {n χ α } ≡ n χ α , n χ α , . . . , n χ α , . . . :=  1 (aχi αi )n χi αi | F  i i 1 1 2 2 i i  n χi αi ! i i

(4.31) where mode index i ∈ N is finite. Orthonormality relations are, {n χ α }|{m χ  α  } = δn χ α m χ  α  δχ χ  δα α  .

(4.32)

4.1 Bosonic Group Field Theory

69

The number operator for a single mode Nχ α = aχ† α aχ α , counts its occupation number   Nχ j α j {n χi αi } = n χ j α j {n χi αi } while the total number operator N =

χ,  α

(4.33)

Nχ α , counts the total number of particles,

⎛   N {n χ α } = ⎝ n χ i i

⎞ j jα

 ⎠ {n χi αi } .

(4.34)

j

4.1.3 Weyl Algebra Operator norm is not defined on the *-algebra A F , because of the unboundedness of the bosonic ladder operators ϕ and ϕ † [51]. As is standard practice in algebraic treatments of many-body quantum systems, we could work instead with exponentiated versions of these resulting in a unital C*-algebra, the Weyl algebra. The following Weyl reformulation of the GFT system is based on the well-known literature in algebraic quantum field theory [50, 51, 61, 62]. For the purposes of this thesis, this surrounds the Fock representation of many-body, non-relativistic systems, here suitably adapted to define an analogous setup for group field theory [29, 30]. The fields ϕ and ϕ † are operator-valued distributions. The corresponding operators are defined by smearing them with functions7 f ∈ H,  ϕ( f ) :=  ϕ†( f ) =

G d ×Rn

G d ×Rn

 g , φ)  d g d φ f¯( g , φ)ϕ(

(4.35)

 † (  . d g d φ f ( g , φ)ϕ g , φ)

(4.36)

Depending on the investigation at hand, the smearing functions may also be required to satisfy additional decay properties (see for instance, Eq. (5.160) in Sect. 5.3.4). The commutation relations (4.10) take the following form, [ϕ( f 1 ), ϕ † ( f 2 )] = ( f 1 , f 2 )

(4.37)

†

[ϕ( f 1 ), ϕ( f 2 )] = [ϕ ( f 1 ), ϕ ( f 2 )] = 0

(4.38)

 f 2 (  d g d φ f¯1 ( g , φ) g , φ)

(4.39)

†



where ( f1 , f2 ) =

G d ×Rn

is the L 2 -inner product. 7

Naturally, the smearing is independent of basis, i.e. ϕ( f ) = a( f ).

70

4 Group Field Theory

Bosonic ladder operators are unbounded in the operator norm on H F , and they are defined on dense subsets of H F . Therefore, let us define the following self-adjoint operators8 in the common dense domain of ϕ and ϕ † , 1 ( f ) := √ (ϕ( f ) + ϕ † ( f )) 2 1

( f ) := √ (ϕ( f ) − ϕ † ( f )) i 2

(4.40) (4.41)

and consider their exponentiations, W F ( f ) := ei ( f )

(4.42)

F ( f ) = ei ( f ) . Then, these exponential operators: or equivalently9 W • are unitary, W F ( f )† = W F ( f )−1 = W F (− f ) , and i • satisfy Weyl relations, W F ( f 1 )W F ( f 2 ) = e− 2 Im( f1 , f2 ) W F ( f 1 + f 2 ). In other words, {W F ( f ) | f ∈ H} defines a Weyl system [50, 51, 63] on the Hilbert space H F , over the space of test functions f . It defines a unitary representation of the GFT commutation algebra on H F with generators . Retaining this algebraic structure and forgetting (for now) the generators which lend the concrete representation, an abstract bosonic GFT system can be defined by the pair (A, S), where A is the Weyl algebra10 generated by Weyl unitaries W ( f ), and S is the space of algebraic states.11 The defining relations of this algebra are, W ( f 1 )W ( f 2 ) = W ( f 2 )W ( f 1 ) e−i Im( f1 , f2 ) = W ( f 1 + f 2 ) e− 2 Im( f1 , f2 ) i

(4.43)

where identity is I = W (0), and unitarity is W ( f )−1 = W ( f )† = W (− f ). This is a unital C*-algebra, equipped with the C*-norm. The benefits of defining a quantum GFT system with an abstract Weyl algebra stem from the fact that some general results can be deduced, which are representation-independent (and would apply, for example, also to other inequivalent representations [26, 30]). This allows in particular for exploring structural symmetries at the level of the algebra formulated in terms of automorphisms. In the upcoming Sect. 4.1.4, we will consider examples of automorphisms of A corresponding to structural symmetries (translations) of the underlying theory. The KMS condition with respect to these automorphisms will then lead to a definition of structural equilibrium states in Sect. 5.1.2.1, which encode In terms of operators and , the commutation relations take the form, [ ( f 1 ), ( f 2 )] = i Re( f 1 , f 2 ), [ ( f 1 ), ( f 2 )] = [ ( f 1 ), ( f 2 )] = i Im( f 1 , f 2 ). 9 Since ( f ) = (i f ), both ϕ and ϕ † can be recovered from or alone. By convention then, are usually chosen as the generators of this representation [51]. 10 Fermionic statistics would correspond to a Clifford algebra. 11 Recall that algebraic states are linear, positive, normalised, complex-valued functionals over an algebra (see footnote 6, on p. 24). 8

4.1 Bosonic Group Field Theory

71

stability with respect to the corresponding internal flows of the transformation under consideration. The Fock system is now generated as the Gelfand-Naimark-Segal (GNS) representation [50, 51, 62, 64] (π F , H F ,  F ) of the regular Gaussian algebraic state given by ω F [W ( f )] := e−

|| f ||2 4

.

(4.44)

Here H F is the GNS representation space which is identical to the one that we constructed in the previous section directly using the ladder operators, via the following identities (4.45) π F (W ( f )) = W F ( f ) = ei ( f ) for all W ( f ) ∈ A. The vector state  F is the cyclic GNS vacuum generating the dense

representation space, π F (A) | F  ⊂ H F . It is the same degenerate Fock vacuum that was introduced earlier, the no-space state. The kinematic system can thus be defined by a pair consisting of, the algebra of bounded linear operators12 B(H F ) on the Fock space or the algebra A F , both of which we encountered before in Sects. 3.1 and 4.1.1; and, the space of normal states Sn over the algebra. Normal states are algebraic states ωρ induced by density operators ρ on H F , i.e. ωρ [A] = Tr(ρ A).

4.1.4 Translation Automorphisms In Sect. 5.1.2 we will construct Gibbs states which are at equilibrium with respect to translations of the system along the base manifold, for which the relevant definitions and constructions are presented below [29].

4.1.4.1

Rn -Translations

The natural translation map on n copies of the real line,  g , φ ) → ( g , φ + φ) Tφ : G d × Rn → G d × Rn , (

(4.46)

induces a linear map (over C) on square-integrable functions as a shift to the right, g , φ ) → (Tφ∗ f )( g , φ ) := ( f ◦ T−φ )( g , φ ) . Tφ∗ : f (

(4.47)

The von Neumann algebra B(H F ) is the closure of the C*-algebra π F (A) in the weak operator topology on H F . Weak operator topology is defined by continuity of the map B(H F )  A → (Aψ1 , ψ2 ), for every ψ1 , ψ2 ∈ H F . Further, the weak operator topology is weaker (or coarser) than the strong operator topology i.e. continuity of the map B(H F )  A → ||Aψ||, for every ψ ∈ H F . Thus, B(H F ) is also strongly closed [61, 62].

12

72

4 Group Field Theory

This is a regular, unitary representation of Rn on H [59, 65]. Notice that Tφ∗ preserves

the L 2 inner product due to translation invariance of the Lebesgue measure, i.e. for any φ ∈ Rn , (Tφ∗ f 1 , Tφ∗ f 2 ) = ( f 1 , f 2 ). Notice also that Tφ∗ is linear on the space of functions f , i.e. for any z 1 , z 2 ∈ C, we have Tφ∗ (z 1 f 1 + z 2 f 2 ) = z 1 Tφ∗ f 1 + z 2 Tφ∗ f 2 . Then, let us define a linear map on the Weyl algebra, αφ : A → A, W ( f ) → W (Tφ∗ f ) .

(4.48)

For each φ, the map αφ defines a *-automorphism of A, and the set of maps {αφ }φ∈R forms a 1-parameter group. This defines a representation α of the group R in the group of automorphisms of the algebra Aut(A), i.e. the map α : R → Aut(A), φ → αφ preserves the algebraic structure of reals, αφ1 +φ2 = αφ1 αφ2 . Extending this to Rn , the maps {αφ }φ∈R  n now form an n-parameter group, and α defines a representation of Rn in Aut(A). See Appendix 1 for details.

4.1.4.2

G d -Left Translations

The natural left13 translations on a group manifold are diffeomorphisms from G to itself. On G d , it is given by the smooth map,  → (  := (g1 g1 , . . . , gd gd , φ)  g  , φ) g . g  , φ) L g : (

(4.49)

which induces a map on the space of functions,  := ( f ◦ L g−1 )(  . g  , φ) g  , φ) L ∗g f (

(4.50)

This is a left regular, unitary representation of G d on H [59, 65]. Notice that L ∗g preserves the L 2 -inner product, i.e. for any g ∈ G d , (L ∗g f 1 , L ∗g f 2 ) = ( f 1 , f 2 ), using left-translation invariance of Haar measure on G d . Also notice that L ∗g is linear on the space of functions f , i.e. for any z 1 , z 2 ∈ C, we have L ∗g (z 1 f 1 + z 2 f 2 ) = z 1 L ∗g f 1 + z 2 L ∗g f 2 . With this, let us define a linear transformation on the Weyl generators, αg (W ( f )) := W (L ∗g f ) .

(4.51)

Then, map αg defines a *-automorphism of A. Also like for Rn -translations, α : G d → Aut(A) is a representation of G d in the group of all automorphisms of the algebra as it preserves the algebraic structure, αg.g = αg αg . See Appendix 1 for details.

13

Analogous statements hold for right translations.

4.1 Bosonic Group Field Theory

4.1.4.3

73

Unitary Representation

Using the following known structural properties of GNS representation spaces [50, 64], the automorphisms defined above can be implemented by unitary transformations in the Fock space H F as follows. α-Invariant state. Let ω be an α-invariant state, i.e. ω[α A] = ω[A] for all A ∈ A, for some α ∈ Aut(A). Then it is known that [50, 64], α is implemented by unitary operators Uω in the GNS representation space (πω , Hω , ω ), defined by Uω πω (A) Uω† = πω (α A) with invariance of the GNS vacuum Uω ω = ω . Similarly, for the general case when ω is invariant under a group of automorphisms, then αg (g ∈ G) is implemented by a unitary representation Uω of G in Hω , such that Uω (g) πω (A) Uω† (g) = πω (αg A) , Uω (g)ω = ω .

(4.52)

Fock state. We recall that the algebraic Fock state over A is given by Eq. (4.44), with the associated GNS representation (π F , H F ,  F ). Then, any automorphism on A that is defined via a norm-preserving transformation on H will leave ω F invariant. Thus ω F is invariant under the class of norm-preserving transformations of the square-integrable test functions, including the translation automorphisms of the base manifold as defined above. Thus, automorphisms αφ and αg are implemented by groups of unitary operators in H F . From the unitary transformations (4.52) as applied to Weyl generators in the Fock representation π F , it is straightforward to see that the group field operators transform in a familiar way,  F (φ )−1 = ϕ( g , φ)U g , φ + φ ) U F (φ )ϕ(  F (  g  )ϕ( g , φ)U g  )−1 = ϕ( g  g, φ) U F (

(4.53) (4.54)

with analogous expressions for their adjoints. From here on the subscript F on the unitary implementations of these translation automorphisms will be dropped with the understanding that in this setting U refers only to the unitary representation of some group in target space U(H F ) of unitary operators on Fock space. We remark that these transformations, defined here for π F (A), being bounded can also be extended to B(H F ). Further, it is important to note (for subsequent use in Sect. 5.1.2.1) that the corresponding group homomorphism U : G d → U(H F ), is strongly continuous in the Fock space. See Appendix 2 for details. Therefore, the system is now equipped with strongly continuous groups of unitary operators in the Fock representation that implement internal shifts of the underlying base manifold G d × Rn .

74

4 Group Field Theory

4.2 Deparametrization in Group Field Theory We have recalled the fundamental difficulties in defining equilibrium in generally covariant systems, due to the absence of preferred time variables in the previous chapters. A general strategy to solve those issues, in the description of the dynamics of such systems is to use matter degrees of freedom as relational clocks, under suitable approximations, and recast the general covariant dynamics in terms of a physical Hamiltonian associated with them. Here also we can consider the same general strategy as a way to tackle our (related) issue of defining statistical equilibrium states in quantum gravity. That is, we can consider the construction of states which are at equilibrium with respect to relational clocks, as will be done in Sect. 5.1.2.2. For this then, we first need to consider in detail aspects of deparametrization in group field theory to define a clock variable, which is the content of this section. Based on insights and tools of presymplectic mechanics as presented in Sect. 2.1, below we lay out the essentials for group field theory. As we will see, the resultant deparametrized, relational system will be ‘canonical’ in clock time which now foliates the original GFT system discussed up until now. Algebra brackets (4.10) will be replaced with the corresponding equal-clock-time commutation relations, analogous to the equal-time commutation relations in a non-covariant system. Our interest in such a setup is natural because GFTs lack a preferred choice of an evolution parameter. The base space G d × Rn is chosen so as to facilitate a relational description of the system by coupling n scalar fields [35]. However, there are n possible variables to choose from, and none is preferred over the others. By construction then, GFTs have a multi-fingered relational time structure in this sense. The way we approach the task of deparametrizing is as follows [29]. We focus first on the classical description in Sect. 4.2.1, starting with the case of a single group field particle in Sect. 4.2.1.1 and sketch how deparametrization works at this simple level, assuming that the GFT dynamics amounts to a specific choice of a scalar Hamiltonian constraint. Then in Sect. 4.2.1.2, we consider the extension of the same deparametrization procedure for a system of many such particles, assumed as noninteracting. We then consider the quantisation of the resulting deparametrized system of many group field particles, arriving at the corresponding quantum multi-particle system in Sect. 4.2.2, which is canonical with respect to a clock time (with respect to which one can then define relational equilibrium, in Sect. 5.1.2.2). Below we sketch the relevant steps of the overall construction [29], and leave a more detailed analysis of the corresponding mathematical structures for GFTs to future work.

4.2.1 Classical System We begin with the investigation of deparametrization for a classical system [29], utilising the framework of extended phase space and presymplectic mechanics as discussed in Sect. 2.1. Here, we face a similar issue of background independence

4.2 Deparametrization in Group Field Theory

75

with the associated absence of a preferred evolution parameter. The reason for undertaking classical considerations first is to utilise the existing knowledge already wellpositioned to be imported to GFT due to the common structures encountered in any such multi-particle system, namely an extended symplectic phase space with a set of constraints, including a dynamical Hamiltonian one.

4.2.1.1

Single-Particle

The extended classical configuration and phase space for the single-particle sector in group field theory is Cex = G d × Rn  (g I , φ a ) ex = T ∗ (Cex ) ∼ = G d × Rn × g∗d × Rn  (g I , φ a , X I , pφ a )

(4.55) (4.56)

where, g is the Lie algebra of G and g∗ is its dual vector space. Here, by a classical particle we mean a point particle living on the group base manifold, thus being described by a point on its phase space. States and observables are respectively points and smooth functions on ex . Statistical states are smooth positive functions on the phase space, normalised with respect to the Liouville measure. The Poisson bracket on the space of observables defines its algebra structure. The symplectic 2-form on ex is,  dpφ a ∧ dφ a (4.57) ωex = ωG + a

where ωG is a symplectic form on T ∗ (G d ). Let us assume that the covariant14 dynamics of this simple system is encoded in a smooth constraint function Cfull : ex → R ,

(4.58)

and that there are no additional gauge symmetries. A single classical particle of the group field is thus described by (ex , ωex , Cfull ). The null vector field is defined by, ωex (YCfull ) = −dCfull

(4.59)

while the constraint surface  is characterised by Cfull = 0, with its presymplectic form given by, ω = ωex | . The null orbits of ω are the graphs of physical motions encoding unparametrized correlations between the dynamical variables of the theory. These gauge orbits are integral curves of the vector field YCfull , satisfying the equations of motion (4.60) ω (YCfull ) = 0 . 14

Throughout Sects. 4.2.1 and 4.2.2, by ‘covariant’ we simply mean ‘not deparametrized’, without any relation to diffeomorphisms on spacetime.

76

4 Group Field Theory

The set of all such orbits is the physical phase space phy that is projected down from  and is equipped with a symplectic 2-form induced from . Then (phy , ωphy ) is the space of solutions of the system and a physical flow means a flow on this space. We notice again that here, a canonical time or clock structure is lacking, and is not required a priori. Deparametrizing this classical system, with respect to, say, the cth scalar field φ c , means reducing the full system to one wherein the field φ c acts as a good clock. As anticipated in Sect. 2.1, this entails the following two separate approximations to Cfull , ˜ I , φ a , X I , pφ α ) Cfull (g I , φ a , X I , pφ a ) ≈ pφ c + C(g α

≈ pφ c + H (g , φ , X I , pφ α ) I

(4.61) (4.62)

where the fixed index c denotes ‘clock’, and index α ∈ {1, 2, . . . , n − 1} runs over the remaining scalar field degrees of freedom that are not intended to be used as clocks and remain internal to the system. The first approximation retains terms up to the first order in clock momentum. At this level of approximation the part denoted by C˜ is a function of the clock time φ c . These two features mean that at this level of approximation φ c behaves as a clock, but only locally since its momentum is not necessarily conserved in the clock time. Furthermore, by linearising in pφ c , we have fixed a reference frame defined by the physical matter field φ c . At the second level, C˜ is approximated by a Hamiltonian H that is independent of φ c , so that on-shell (i.e. pφ c = −H ) we have conservation of the clock momentum ∂φ c p φ c = 0 .

(4.63)

H generates relational dynamics in φ c , which now acts as a global clock for this deparametrized system. We thus have a new system (ex , ωex , Cdep ) after the above approximations, with Cdep = pφ c + H (g I , φ α , X I , pφ α )

(4.64)

now deparametrized with respect to one of the extended configuration variables φ c which takes on the role of a good clock variable. See also Eq. (2.10) and the surrounding discussion. The presymplectic setup of this deparametrized system now takes on a structure mirroring that of a parametrized non-relativistic particle with a well-defined time. The constraint surface defined by vanishing of the relevant constraint, here Cdep = 0, now admits the topology of a foliation in clock time,  = R × can  (φ c , g I , φ α , X I , pφ α ) .

(4.65)

As we have noticed before, this form of  is a characteristic feature of a system with a clock structure. The reduced, canonical configuration and phase spaces are now

4.2 Deparametrization in Group Field Theory

77

given by, Ccan = G d × Rn−1 , ∗

(4.66) α

can = T (Ccan )  (g , φ , X I , pφ α ) . I

(4.67)

The function H : can → R is the clock Hamiltonian encoding relational dynamics in φ c , and one can subsequently define the standard Hamiltonian dynamics with respect to it.

4.2.1.2

Multi-particle

We now want to extend the above deparametrization procedure beyond the oneparticle sector. Let us consider the simplest case of two, non-interacting particles [29, 66, 67]. Let (1,2) )  (g (1,2)I , φ (1,2)a , X (1,2) , pφ(1,2) )  (1,2) = T ∗ (Cex a I

(4.68)

be the extended phase spaces of particles 1 and 2 respectively. The extended phase space of the composite system is  =  (1) ×  (2)

(4.69)

with symplectic 2-form ω = ω(1) + ω(2) . Notice that each particle is equipped with n possible clocks. The aim is to select a single common clock for the composite system so as to then be able to define a common equilibrium for the total system. (1,2) : Let the individual dynamics of each particle be given by constraints Cfull (1,2) (1)c1 → R. Deparametrizing particle 1 with respect to say variable φ , and par ticle 2 with respect to say a different φ (2)c2 , gives the new constraints for each, (1) C (1) = pφ(1)c1 + H (1) (g (1)I , φ (1)α , X (1) I , pφ α )

C

(2)

=

pφ(2)c2

+H

(2)

(g

(2)I

,φ

(2)α

,

X (2) I ,

pφ(2)α )

(4.70) (4.71)

where H (1,2) are functions on the individual reduced phase spaces, (1,2) (1,2) = T ∗ (Ccan )  (g (1,2)I , φ (1,2)α , X (1,2) , pφ(1,2) ) can α I

(4.72)

with symplectic 2-forms, (1,2) = ωG(1,2) + ωcan

 α

dpφ(1,2) ∧ dφ (1,2)α . α

(4.73)

78

4 Group Field Theory

This is a complete theoretical description of the deparametrized 2-particle system. However, it is inconveniently described in terms of two different clocks ascribed to each particle separately. We are seeking a single common clock. Such a clock can be defined by synchronizing the two individual clocks, via the imposition of an additional constraint as follows. Let us choose φ (1)c1 to be the common clock, and write the second clock as a smooth function of the first, that is φ (1)c1 = t , φ (2)c2 = F(t) .

(4.74)

More generally, we can choose a common clock t ∈ R, and sync the two separate clocks with it via two functions, Fi : t → φ (i)ci , i = 1, 2 .

(4.75)

Any such syncing function, which maps two clocks, is assumed to be a bijection. It is thus invertible. This is done to ensure that the procedure of syncing is consistent and well-defined. Say, clock 2 is synced with clock 1. What we mean by this is that, every reading from clock 2 should give a unique reading of clock 1. This is possible only if the map between the readings, that is F, is one-to-one and onto. We work with the case associated with Eq. (4.74), for simplicity. Then, syncing the two clocks can be imposed by a constraint of the form,15 s := φ (1)c1 − F −1 (φ (2)c2 ) .

(4.76)

Imposing this constraint, i.e. s = 0, amounts to choosing a 1-parameter flow in the (here, 2-dim) space of the clock variables φ (1)c1 and φ (2)c2 , which can themselves be understood as gauge parameters due to their association with dynamical constraints C (1) and C (2) . Thus, this syncing can be seen as gauge fixing [66, 67]. Then the gauge-fixed 2-form of  is,

where,

ω˜ := ω|s=0 = ωcan + dpt ∧ dt

(4.77)

pt = pφ(1)c1 + F  (t) pφ(2)c2

(4.78)

is the clock momentum of the single clock t, and (1) (2) + ωcan ωcan = ωcan

(4.79)

(1) (2) × can of is the symplectic form on the canonical reduced phase space can = can  the composite system. Here, prime denotes a total derivative with respect to t.

15

In the more general case with two functions F1 and F2 , the syncing constraint can be given by, s = F1−1 (φ (1)c1 ) − F2−1 (φ (2)c2 ). In this case, the common clock is t = F1−1 (φ (1)c1 ) = F2−1 (φ (2)c2 ), when this constraint is imposed.

4.2 Deparametrization in Group Field Theory

79

Now, one can consider a reformulation16 of the constraints C (1) and C (2) [66, 67], in terms of (4.80) C := C (1) + C (2) along with,  := C (1) − C (2) . Further, notice that on the constraint surface we have, C (2) = 0 ⇔ F  C (2) = 0, for an arbitrary non-zero function F  . Then, the constraint C can be rewritten as, C˜ := C (1) + F  C (2) . We thus have, C˜ = pt + H (1) + F  (t)H (2)

(4.81)

where the Hamiltonian H (1) + F  (t)H (2) is independent of clock t iff F  (t) = k, for k an arbitrary non-zero real constant. In other words, t is a good clock for the choice ˜ This gives, of affine gauge F(t) = kt + k.

where,

C˜ = pt + H

(4.82)

H = H (1) + k H (2) .

(4.83)

Now that the 2-particle system has been brought to the form of a standard Hamiltonian system with clock time t, the remaining elements for the complete extended symplectic description can be identified. The extended configuration and phase spaces are Cex = R × Ccan  (t, g (1)I , φ (1)α , g (2)J , φ (2)γ ) ex = T ∗ (Cex )

(4.84) (4.85)

˜ The constraint function C˜ defines the presymplectic surface with ωex = ω. (1) (2) (2)J , φ (2)γ , X (2)  = R × can  (t, g (1)I , φ (1)α , X (1) I , pφ α , g J , pφ γ )

(4.86)

with ω = ωcan − d H ∧ dt .

(4.87)

˜ as given above provides a complete description of the 2-particle Thus, (ex , ωex , C) non-interacting system equipped with a single relational clock t. For an N -particle non-interacting system, each with n possible clocks, the extension of the above procedure is direct. Select any one φ variable as a clock for each individual particle, i.e. bring the individual full constraints of each particle to deparametrized forms like in (4.71). Then, given one clock per particle, identifying a global clock for all particles means choosing any one at random (call it t) and synchronizing the rest with this one via affine functions F2 (t), . . . , FN (t). This defines a relational system on Cex  (t, g (1)I , φ (1)α , . . . , g (N )J , φ (N )γ ), ex = 16

We have that {C (1) = 0, C (2) = 0} ⇔ {C = 0,  = 0}.

80

4 Group Field Theory

T ∗ (Cex ), with constraint function C˜ = pt + H on ex , and Hamiltonian function H = H (1) + k2 H (2) + · · · + k N H (N ) on can .

4.2.1.3

Discussion

Before moving on to quantisation, let us pause to make a few important remarks, and summarise Sects. 4.2.1.1 and 4.2.1.2 [29]. The following discussion is meant to: 1. clarify that we are dealing with two different, ‘before’ and ‘after’ deparametrization, systems. The former is covariant (or constrained), while the latter is derived from the former via the deparametrization approximations in Eqs. (4.61)–(4.62). In general the two systems are physically distinct. However, it is possible that deparametrization does not change the physical content of the theory. This corresponds to the case in which the deparametrization steps in (4.61)–(4.62) do not correspond to approximations of the dynamics, but to an exact re-writing of it, e.g. a relativistic particle (see Sect. 2.1.2 for simple illustrative examples); 2. clarify that the latter, ‘after’ deparametrization, system, includes within it a canonical system, which is eventually quantised. This system is ‘canonical’ (or nonrelativistic, see Sect. 2.1) with respect to the relational clock that is selected during the process of deparametrization; 3. clarify the conceptual (and notational) differences between these systems. For the 1-particle system the ‘before’ picture is one wherein the system is fully covariant and the corresponding kinematics consist of the configuration space cov cov cov = G d × Rn  (g I , φ a ) and phase space ex = T ∗ (Cex ). Covariant (or conCex strained) dynamics is encoded in a dynamical constraint function Cfull defined on cov cov . Vanishing of the constraint function defines a constraint hypersurface in ex . ex The ‘after’ picture defines the second system, which includes the canonical one. dep The extended configuration space of the deparametrized system is Cex = R × (G d × n−1 I α R )  (t, g , φ ), where the 1-particle canonical configuration space is Ccan = G d × Rn−1 . Here, we have denoted φ c ≡ t. Canonical variables are those dynamical cov which are not used as clocks. The variables of the original covariant system Cex dep dep extended phase space is ex = T ∗ (Cex ). Deparametrized dynamics is encoded in dep a constraint function C on ex , of the form, C = pt + H , where H is a smooth function on the canonical phase space can = T ∗ (Ccan ).17 It is a genuine Hamiltonian defining dynamical evolution with respect to the relational clock t. The constraint surface (satisfying C = 0) is  = R × can , characterised by a foliation consisting of slices can along clock t. This form of  and the existence of the canonical subsystem is a direct consequence of deparametrization. The canonical subsystem is thus absent cov cov , ωex , Cfull ). for a generic non-deparametrized, constrained system (ex Note that for the 1-particle system, the covariant and deparametrized kinematic dep cov = G d × Rn and Cex = R × descriptions, in the respective configuration spaces Cex d n−1 (G × R ), are identical. As will be seen below, this does not hold for an N -particle 17

See Eq. (4.64), or (2.15).

4.2 Deparametrization in Group Field Theory

81

system with N > 1, when seeking a description with a single clock. In this case, the dep cov = (G d × Rn )×N and Cex,N = R × (G d × Rn−1 )×N . configuration spaces are Cex,N For the non-interacting N -particle system, the ‘before’ system concov = (G d × Rn )×N  sists of the covariant extended configuration space Cex,N cov cov (1)I (1)a (N )J (N )b ,φ ) and the associated phase space ex,N = T ∗ (Cex,N )= (g , φ , . . . , g (1) (N ) cov ×N (ex ) . The covariant dynamics is encoded in a set of constraints Cfull , . . . , Cfull , each defined on the respective copies of the 1-particle covariant extended phase space cov . ex The ‘after’ system is deparametrized with a single clock t. As before, existence of this clock structure means that the extended symplectic description takes on the form dep of a non-relativistic system. The extended configuration space is Cex,N = R × Ccan,N where the N -particle reduced configuration space is Ccan,N = (G d × Rn−1 )×N , and the clock t ∈ R is an extended configuration variable. The extended phase space of dep dep the deparametrized system is ex,N = T ∗ (Cex,N ). The deparametrized dynamics is encoded in a constraint function, C N = pt + H N dep

defined on ex,N . Constraint surface  = R × can,N is characterised by C N = 0. The canonical phase space is can,N = T ∗ (Ccan,N ). Relational dynamics is encoded in the clock Hamiltonian defined on can,N given by, HN =

N 

ki H (i) ,

(4.88)

i=1

for arbitrary real non-zero constants ki which encode the rates of synchronization between the N different clocks, one per particle. Functions H (i) are single-particle clock Hamiltonians defined on the respective copies of single-particle reduced phase space can . We can already anticipate that relational canonical Gibbs states are those that are KMS with respect to the t-flow of a clock Hamiltonian HN . Finally, notice the similarity in the form of HN in Eq. (4.88) above, and the modular Hamiltonian with respect to a given set of observables in Eq. (2.36). Based on the above discussion, one can understand the generalised temperatures βa in the latter as the rates at which the individual modular flow parameters, each associated with a different Oa , sync with each other, in the case when there exists a single clock corresponding to the single constraint in Eq. (2.54).

4.2.2 Quantum System We now move on to the quantisation of the above deparametrized non-interacting, many-body system. Our treatment is again limited to outlining the basic steps, which

82

4 Group Field Theory

is sufficient at least for our present purposes [29]. In the context of deparametrization, since we are primarily interested in scalar degrees of freedom residing in copies of R, we will continue to be content with omitting rigorous details about the symplectic structure on T ∗ (G), and its subsequent quantisation to a commutator algebra. We shall also not choose any specific quantisation map, and focus on the general ideas required to eventually define a φ-relational Gibbs state. Further details can be found in [68], including examples of quantisation maps for T ∗ (G). Quantisation maps the phase space to a Hilbert space, and the classical algebra of observables as smooth (real) functions on the phase space to (self-adjoint) operators on the Hilbert space, with the Poisson bracket on the former being mapped to a commutator bracket on the latter.

4.2.2.1

Single-Particle

cov = T ∗ (G d × Rn ) maps to, For the covariant 1-particle system, the phase space ex

H ≡ Hcov = L 2 (G d × Rn )

(4.89)

cov = G d × Rn . This is the Hilbert defined over the extended configuration manifold Cex space of a single quantum of geometry that we presented in earlier sections. Observcov , which map to operators ables are the algebra of real-valued smooth functions on ex on H, with the Poisson structure on the former being mapped to the Heisenberg algebra on the latter. Specifically, for the matter degrees of freedom, this is

pφ b ] = iδab {φ a , pφ b } = δab  [φa , 

(4.90)

where the hat denotes some quantisation map. Notice here that all n scalar fields are quantised. This is in contrast with the corresponding case of the canonical system, wherein the canonical phase space can = T ∗ (G d × Rn−1 ) maps to a canonical Hilbert space, (4.91) Hcan = L 2 (G d × Rn−1 ) with the algebra again mapping from functions on can to operators on Hcan . But now, the brackets defining the algebra structure of the system are reduced by one in number, as a direct consequence of the reduction of the base space by one copy of R, to which the clock variable belongs. Under quantisation we now have, α ,  pφ γ ] = iδαγ {φ α , pφ γ } = δαγ  [φ

(4.92)

where α, γ = 1, . . . , n − 1. The commutator corresponding initially to the clock φ-variable is now identically zero, that is [φc , p φc ] = 0 ,

(4.93)

4.2 Deparametrization in Group Field Theory

83

meaning that the corresponding degrees of freedom are treated as entirely classical; moreover, their intrinsic dynamics is trivialised. In other words, this quantum canonical system is one in which there exists a classical clock, which was quantum in the original quantum covariant system. Dynamics is defined via a Hamiltonian operator Hˆ on Hcan giving evolution with respect to the clock.

4.2.2.2

Multi-particle

cov cov ×N = (ex ) is mapped to For the covariant N -particle system, ex,N

H N = H⊗N .

(4.94)

cov is mapped to an operator algebra on H N , Algebra of smooth functions on ex,N whose quantum matter fields now satisfy

 ( j) [ φ (i)a , pφ b ] = iδab δi j

(4.95)

where i, j = 1, 2, . . . , N denote the particle label. This is the multi-particle sector as considered in Sects. 3.1 and 4.1.1. Again, we note that none of the N particles have chosen a clock yet, that is all n × N number of scalar fields φ are quantum. In the corresponding canonical quantum system ⊗N Hcan,N = Hcan

(4.96)

with the algebra of observables on it, the single clock variable t (which is synced with all the separate clocks now carried by each particle) is classical. The Hamiltonian operator defining t-evolution, for fixed N , is given by the operator Hˆ N =

N 

ki Hˆ (i)

(4.97)

i=1

where Hˆ (i) are the separate Hamiltonians of each particle scaled by the respective rates of syncing of the different clocks (or, generalised inverse temperatures [69]), and we have neglected interactions. In the multi-particle case, it is worthwhile to also look at the quantised extended dep dep deparametrized system. This consists of ex,N being quantised to H N = L 2 (R × Ccan,N ) and the corresponding Heisenberg algebra has two additional generators (compared to the canonical system) satisfying [ t,  pt ] = i. Such a system is different from both the quantum extended covariant and the quantum canonical. In the former, there is no single clock variable. In the latter, there is one but it is no longer quantum. Quantising the extended deparametrized system is like quantising a non-relativistic particle at the level of its extended phase space, which includes Newtonian time and

84

4 Group Field Theory

its conjugate momentum as phase space variables. Quantising Newtonian time to define the corresponding operator comes with its own set of conceptual and technical problems. However our case is fundamentally different because here t is really a function of degrees of freedom that are understood as coupled scalar matter fields [35]. Therefore for a multi-particle system, one ends up with three different quantum systems: quantum extended covariant, quantum extended deparametrized and quantum canonical. The last two each have a potential clock parameter, and going from the former to the latter is the step of making this variable classical and therefore treating it as a perfect, thus idealised, clock. This distinction between quantum extended covariant and extended deparametrized systems is absent in the simple 1-particle system because in this case deparametrization does not require the extra step of syncing the different clocks (as there is only one). It only requires choosing one out of n so that the kinematics of both systems ends up being identical.

4.2.2.3

Fock Extension

We arrive now at the quantum Fock systems built out of the above N -particle systems. The covariant Fock system composed of the N -particle quantum extended covariant systems as described above is the GFT Fock representation as detailed in Sect. 4.1. On the other hand, a canonical Fock system (associated with a degenerate vacuum) is as follows. The canonical Hilbert space for bosonic quanta can be identified as Hcan,F =



⊗N sym Hcan ,

(4.98)

N ≥0

which is generated by ladder operators acting on a cyclic vacuum, and satisfying the equal- (Fock-) clock-time commutation relations, g , g )δ(φ − φ  ) [ϕ(t ˆ F , g, φ), ϕˆ † (t F , g , φ  )] = I(

(4.99)

with [ϕ, ˆ ϕ] ˆ = [ϕˆ † , ϕˆ † ] = 0, and I and δ being the respective delta distributions on G d n−1 and R . Notation · has been used to make explicit the difference between variables φ in canonical and covariant systems. Here φ ≡ (φ 1 , . . . , φ n−1 ) denotes canonical variables whereas earlier, φ ≡ (φ 1 , . . . , φ n ) belonged to the covariant system in which all scalar fields were internal variables. g continues to denote (g1 , . . . , gd ). The associated canonical Weyl system is now based on test functions which are defined on the reduced configuration space Ccan = G d × Rn−1 , and analogous constructions to those considered in Sect. 4.1.3 follow through. The *-algebra Acan,F now consists of polynomial functions of the above canonical ladder operators, defined over the reduced base space G d × Rn−1 . For example, the number operator now takes the form,  ˆ d g dφ ϕˆ † ( g , φ)ϕ( ˆ g , φ) . (4.100) N= G d ×Rn−1

4.2 Deparametrization in Group Field Theory

85

Note that one can understand these quantities also as observables in the full theory, just computed at given values of the relational clock variable. The heuristic interpretation is valid, but the actual algebraic properties of these observables would be (potentially very) different. Particularly, from the point of view of the original non-deparametrized system described by the algebra (4.10), one can already expect quantities in a φ-frame to have singularities due to the presence of limφ→φ  δ(φ − φ  ). As we will see in Sect. 5.2, this feature is unavoidable in aspects of inequivalent thermal representations induced by generalised Gibbs states, and their subsequent applications in GFT condensate cosmology. In Sect. 5.3.3 we will also suggest one possible way of introducing nonsingular clock frames, through a class of smearing functions t (φ), and subsequently apply them to derive relational equations of motion for effective homogeneous and isotropic cosmology [47]. Let us make a further remark regarding deparametrization from the perspective of the full quantum non-deparametrized theory. The strategy employed above for a finite dimensional system is to start from a classical constrained system, deparametrize it to get a classical canonical system with respect to a relational clock, and then quantise the canonical system leaving the clock as classical. A more fundamental construction leading possibly to a more physical sort of (approximate) deparametrization is to begin from the complete quantum theory (in our case, a group field theory) in which all possible relational scalar fields are quantum. Then deparametrizing would mean to identify a relevant regime of the full theory in which one of the coupled scalar fields becomes semi-classical, and only then apply the deparametrization approximations outlined in the classical case to our full quantum system. For example, such a regime could be associated with a class of semi-classical coherent states peaking on a specific would-be clock variable [48]. We will briefly return to this point in Sects. 5.3.3 and 5.3.4, when we discuss in detail our setup of using smearing functions to define clock frames as reported in [47]. We leave further investigation of quantum matter reference frames and deparametrization in the present quantum gravitational system to future work [44, 70–75]. Lastly, comparing the algebra (4.99) to (4.10), it is evident that the algebra in (4.99) describes a canonical setup. The nature of the time t F requires clarifications, which we now provide, and more work, which we leave for the future. A canonical Fock system requires a global time variable which is common to all the different multiparticle sectors, that is for a varying N . In other words, a clock variable, extracted somehow from the original covariant system, which in the reduced canonical system plays a role similar to the time in usual many-body quantum physics. In the case of GFTs, as we saw above, this is a relational variable (or a function of several such variables). To get a clock for the canonical Fock system then, one needs a Hamiltonian constraint operator defining some model, since the definition of a relational clock is always model-dependent due to the clock itself being one of the dynamical variables of the full extended system; and the Fock time variable must be accessible from all N -particle sectors, that is its construction and definition must be compatible with changing the total particle number.

86

4 Group Field Theory

To see this, consider a system with two non-interacting particles, each equipped with its own clocks φ c1 and φ c2 , along with their clock Hamiltonians H (1) and H (2) respectively. Let t be the global clock time such that φ c1 = F1 (t) = k1 t + k˜1 and φ c2 = F2 (t) = k2 t + k˜2 . Equivalently, t = F1−1 (φ c1 ) = F2−1 (φ c2 ). The t-clock Hamiltonian is H2 = k1 H (1) + k2 H (2) . Now let’s add a third particle to the mix, such that the resultant system remains non-interacting. Then in the new system, the global clock variable t  will in general be different from t, corresponding to a changed relational dynamics given now by H3 which has a non-zero contribution from the dynamics of the third particle also. However, notice that if this third particle, besides its own clock φ c3 , was also equipped with additional information, namely a syncing function F3 , then it would “know” how to sync with t. Therefore, for an arbitrarily large number N of non-interacting particles, if each is equipped with an individual clock φ ci and a syncing function Fi , then a common clock time can be defined via, t F = F1−1 (φ c1 ) = F2−1 (φ c2 ) = . . .

(4.101)

where, in the present setting as detailed above, the set of functions Fi are essentially put in by hand. In fact, we can expect that this syncing information may naturally be encoded within non-trivial interaction terms [67], the investigation of which we leave to future work.

Appendix 1: *-Automorphisms for Translations We show that the map defined in (4.51) is a *-automorphism of the GFT Weyl algebra with respect to G d translations. Notice that the case G = R, d = n is included within this more general case. Thus, the following proof is also applicable to the map (4.48). Let us first recall the required definitions [50]: Definition. A *-homomorphism between two C*-algebras is a map π : A1 → A2 , which 1. is complex linear π(z 1 A + z 2 B) = z 1 π(A) + z 2 π(B) 2. preserves algebra composition π(AB) = π(A)π(B) 3. preserves *-operation π(A∗ ) = π(A)∗ for all A, B ∈ A1 and z 1 , z 2 ∈ C. The *-operation is what we have denoted as the †-operation throughout this thesis. Definition. A *-isomorphism π is a bijective *-homomorphism, i.e. ker(π ) = {0}. Definition. A *-automorphism α is a *-isomorphism of the algebra into itself, i.e. α : A → A, and ker(α) = {0}.

4.2 Deparametrization in Group Field Theory

87

Lemma 1 Map αg as defined in Eq. (4.51) is a *-homomorphism of the GFT Weyl algebra A. Proof 1. For the Weyl generators, map αg (for every g ∈ G d ) is: composition preserving, αg (W ( f 1 )W ( f 2 )) = αg (W ( f 1 + f 2 ) e− 2 Im( f1 , f2 ) ) i

= αg (W ( f 1 + f 2 )) e

= W (L ∗g ( f 1 + f 2 )) e = =

(4.102)

− 2i Im( f 1 , f 2 ) − 2i Im(L ∗g f 1 ,

(4.103) L ∗g f 2 )

i ∗ ∗ W (L ∗g f 1 + L ∗g f 2 ) e− 2 Im(L g f1 , L g f2 ) W (L ∗g f 1 )W (L ∗g f 2 ) = αg (W ( f 1 )) αg (W ( f 2 ))

(4.104) (4.105) (4.106)

*-operation preserving, αg (W ( f )† ) = αg (W (− f )) = W (−L ∗g f ) = W (L ∗g f )† = (αg W ( f ))† .

(4.107)

αg satisfies linearity over C by definition. These properties are extended to the full algebra by linearity and composition.  Lemma 2 The *-homomorphism αg : A → A is a *-automorphism, i.e. ker(αg ) = {0}. Proof 2. Recall that, for any g ∈ G d , ker(αg ) = {A ∈ A | αg A = 0}. Then, for a generic element A ∈ A, given by a superposition of the basis elements W ( f ), we have   ci W ( f i ) = ci W (L ∗g f i ) (4.108) αg A = αg i

i

where ci ∈ C, i ∈ N. Recall that, L ∗ : G d × H → H is the regular representation of G d on the space of functions H, which is closed under the action of L ∗g (for all g ∈ G d ) [59, 65]. Thus, W (L ∗g f i ) are also elements of the same basis set.18 Then, by using linear independence of the basis, and by definition of element A, we have 

ci W (L ∗g f i ) = 0

⇔

ci = 0 ∀ i

⇔

A = 0.

(4.109)

i

Thus, αg A = 0 ⇔ A = 0.



Lemma 3 Map α : G d → Aut(A) is a representation of G d into the group of all automorphisms of the algebra A. 18

Another simple way to see this is: for a given g ∈ G d , L ∗g f := f ◦ L g−1 , i.e. map L ∗g is a

composition of f with left translations on G d , and these are diffeomorphisms on G d [59, 65].

88

4 Group Field Theory

Proof 3. For any g1 , g2 ∈ G d , we have: g ) = f (( g1 . g2 )−1 . g ) = f ( g2−1 . g1−1 . g ) = (L ∗g2 f )( g1−1 . g ) = (L ∗g1 L ∗g2 f )( g) (L ∗g1 .g2 f )( (4.110) and, (4.111) W (L ∗g1 L ∗g2 f ) = αg1 (W (L ∗g2 f )) = αg1 αg2 (W ( f )) . Then, composition is preserved by α: αg1 .g2 (W ( f )) = W (L ∗g1 .g2 f ) = W (L ∗g1 L ∗g2 f ) = αg1 αg2 (W ( f ))

(4.112)

where, we have used results (4.110) and (4.111). This is extended to the full algebra by linearity and composition. 

Appendix 2: Strong Continuity of Unitary Translation Group The existence of unitary groups in H F has been established in Sect. 4.1.4.3, using the invariance of the Fock state ω F under the translation automorphisms. Given g ) is strongly U ( g ) ∈ U(H F ), for g ∈ G d , we show below that the map g → U ( continuous in H F . Notice that the case G = R, d = n with T ∗ = L ∗ , is included within this more general case. This proof is along the lines of that reported in [29], but is detailed further for clarity. Lemma. {U ( g ) | g ∈ G d } is a strongly continuous family of operators in H F , i.e. g2 ))ψ|| → 0 , as g1 → g2 ||(U ( g1 ) − U (

(4.113)

for all ψ ∈ H F , and all g1 , g2 ∈ G d . Proof. Let us begin with the set of basis vectors {W F ( f ) F | f ∈ H} in H F . Recall: from Eq. (4.45), (4.114) W F ( f ) = π F (W ( f )) , and, from Eqs. (4.52) and (4.51), g )−1 = W F (L ∗g f ) , U ( g ) F =  F . U ( g )W F ( f )U ( Then, for any g1 , g2 ∈ G d ,

(4.115)

4.2 Deparametrization in Group Field Theory

89

||(U ( g1 ) − U ( g2 ))W F ( f )  F ||2 = (U ( g1 )W F ( f )  F , U ( g1 )W F ( f )  F ) + (U ( g2 )W F ( f )  F , U ( g2 )W F ( f )  F ) − (U ( g1 )W F ( f )  F , U ( g2 )W F ( f )  F ) − (U ( g2 )W F ( f )  F , U ( g1 )W F ( f )  F ) (4.116) = ||W F (L ∗g1 f ) F ||2 + ||W F (L ∗g2 f ) F ||2 − 2 Re (W F (L ∗g2 f ) F , W F (L ∗g1 f ) F ) . (4.117) Notice that, for any g ∈ G d , ||W F (L ∗g f ) F ||2 ≤ ||W F (L ∗g f )||2 || F ||2 = ||W F (L ∗g f )||2 = 1

(4.118)

where, the last equality is because W F ( f ) is a unitary operator, for any f (see Eq. (4.45)), and, ||π F (.)|| is the operator norm19 on H F . This implies that, ||W F (L ∗g1 f ) F ||2 + ||W F (L ∗g2 f ) F ||2 ≤ 2 .

(4.119)

Also, notice that, we have (W F (L ∗g2 f ) F , W F (L ∗g1 f ) F ) = ( F , W F (L ∗g2 f )† W F (L ∗g1 f ) F )

(4.120)

= ( F , π F (W (−L ∗g2 f )W (L ∗g1 f )) F ) = ( F , π F (W (−L ∗g2 f + L ∗g1 f )e

(4.121)

− 2i Im(−L ∗g 2

f,L ∗g 1

f)

) F )

(4.122) = ( F , W F (L ∗g1 f − L ∗g2 f )e =e =e

i ∗ 2 Im(L g2

f,L ∗g f )

i ∗ 2 Im(L g2

f,L ∗g 1

1

f)

i ∗ 2 Im(L g2

f,L ∗g f ) 1

F )

ω F [W (L ∗g1 f − L ∗g2 f )] e

−||L ∗g 1

f −L ∗g 2

f ||2 /4

(4.123) (4.124) (4.125)

and its real component,   i ∗ ∗ ∗ ∗ 2 Re (W F (L ∗g2 f ) F , W F (L ∗g1 f ) F ) = Re e 2 Im(L g2 f,L g1 f ) e−||L g1 f −L g2 f || /4

=e

−||L ∗g 1

f −L ∗g 2

f ||

2

(4.126)  1 /4 Im(L ∗g2 f, L ∗g1 f ) . cos 2 (4.127) 

For the functions f , we have 19

For any bounded operator A on H F , the operator norm is ||A|| := sup

∈H F

||A|| |||| .

90

4 Group Field Theory

(L ∗g2 f, L ∗g1 f ) =

 

G d ×Rn



G d ×Rn

= =

G d ×Rn

 g L ∗ f ( d φd g )L ∗g1 f ( g) g2

(4.128)

 g f ( d φd g2−1 . g ) f ( g1−1 . g)

(4.129)

 f (   h f (h) d φd g1−1 . g2 .h)

(4.130)

−→ ( f, f ) = || f ||2

as g1 → g2

(4.131)

where, translation invariance of Haar measure on G d gives equality (4.130), and smoothness of f and of multiplication map on any Lie group gives (4.131). Further, we have, ||L ∗g1 f − L ∗g2 f ||2 = ||L ∗g1 f ||2 + ||L ∗g2 f ||2 − 2Re (L ∗g2 f, L ∗g1 f ) = 2|| f || − 2

2Re (L ∗g2

f,

L ∗g1

f)

as g1 → g2

−→ 0

(4.132) (4.133) (4.134)

using the result (4.131).20 Therefore, for any g1 , g2 ∈ G d :    1 −||L ∗g f −L ∗g f ||2 /4 1 2 ||(U (g1 ) − U (g2 ))W F ( f )  F ||2 ≤ 2 1 − e cos Im(L ∗g2 f, L ∗g1 f ) 2 as g1 → g2

−→ 0

(4.135)

using the results (4.117), (4.119), (4.127), (4.131) and (4.134). Now, consider the dense domain D = Span{W F ( f ) F | f ∈ H} ⊂ H F , and a vector ψ ∈ D written generally as a superposition of the basis vectors, ψ=



ci W F ( f i ) F

(4.136)

i

with coefficients ci ∈ C. Then, we have g2 ))ψ|| ≤ ||(U ( g1 ) − U (



|ci | ||(U ( g1 ) − U ( g2 )) W F ( f i ) F ||

(4.137)

i

−→ 0

as g1 → g2

(4.138)

using the result (4.135) for each i. Thus, the family of unitary operators {U ( g ) | g ∈ G d } is strongly continuous in D. Finally, notice that U ( g ) (for all g ∈ G d ) are bounded linear transformations, thus extended naturally to H F . Also, D is dense in H F , i.e. for every  ∈ H F and arbitrarily small  > 0, ∃ ψ ∈ D such that || − ψ|| < . Then, We remark that results (4.134) and (4.131) basically show strong continuity of representation L ∗ of G d on H. This is an expected feature of regular representations of locally compact Lie groups, on the space of square-integrable smooth functions defined on the same group [59]. 20

4.2 Deparametrization in Group Field Theory

91

||U ( g1 ) − U ( g2 )|| ≤ ||U ( g1 ) − U ( g1 )ψ|| + ||(U ( g1 ) − U ( g2 ))ψ|| + ||U ( g2 )ψ − U ( g2 )|| = 2|| − ψ|| + ||(U ( g1 ) − U ( g2 ))ψ|| < 2 + ||(U ( g1 ) − U ( g2 ))ψ|| < 3 using strong continuity in D for the last inequality.

(4.139) (4.140) (4.141) 

References 1. Hesse MB (2005) Forces and fields: The concept of action at a distance in the history of physics. Dover Publications Inc 2. Ashtekar A, Lewandowski J (2004) Background independent quantum gravity: a status report. Class Quant Grav 21:R53. https://doi.org/10.1088/0264-9381/21/15/R01 3. Rovelli C (2004) Quantum gravity. Cambridge monographs on mathematical physics. Cambridge University Press. https://doi.org/10.1017/CBO9780511755804 4. Bodendorfer N (2016) An elementary introduction to loop quantum gravity. arXiv:1607.05129 5. Perez A (2013) The spin foam approach to quantum gravity. Living Rev Rel 16:3. https://doi. org/10.12942/lrr-2013-3 6. Rovelli C, Vidotto F (2014) Covariant loop quantum gravity: an elementary introduction to quantum gravity and spinfoam theory. Cambridge University Press. https://doi.org/10.1017/ CBO9781107706910 7. Loll R (2019) Quantum gravity from causal dynamical triangulations: a review. Class Quant Grav 37(1):013002. https://doi.org/10.1088/1361-6382/ab57c7 8. Gurau R, Ryan JP (2012) Colored tensor models - a review. SIGMA 8:020 9. Hamber HW (2009) Quantum gravity on the lattice. Gen Rel Grav 41:817–876. https://doi. org/10.1007/s10714-009-0769-y 10. Kotecha I (2019) Thermal quantum spacetime. Universe, 5(8):187. https://doi.org/10.3390/ universe5080187 11. Reisenberger MP, Rovelli C (2001) Space-time as a Feynman diagram: the connection formulation. Class Quant Grav 18:121–140. https://doi.org/10.1088/0264-9381/18/1/308 12. Freidel L (2005) Group field theory: an overview. Int J Theor Phys 44:1769–1783. https://doi. org/10.1007/s10773-005-8894-1 13. Oriti D (2009) The group field theory approach to quantum gravity. In: Oriti D (ed) Approaches to quantum gravity: toward a new understanding of space, time and matter. Cambridge University Press 14. Oriti D (2011) The microscopic dynamics of quantum space as a group field theory. In: Proceedings, foundations of space and time: reflections on quantum gravity: Cape Town, South Africa, pp 257–320 15. Oriti D (2007) Quantum gravity as a quantum field theory of simplicial geometry. In: Fauser B, Tolksdorf J, Zeidler E (eds) Quantum gravity: mathematical models and experimental bounds. Birkäuser, pp 101–126 16. Oriti D (2016) Group field theory as the 2nd quantization of loop quantum gravity. Class Quant Grav 33(8):085005. https://doi.org/10.1088/0264-9381/33/8/085005 17. Bianchi E, Dona P, Speziale S (2011) Polyhedra in loop quantum gravity. Phys Rev D 83:044035. https://doi.org/10.1103/PhysRevD.83.044035 18. Oriti D, Ryan JP, Thuerigen J (2015) Group field theories for all loop quantum gravity. New J Phys 17(2):023042. https://doi.org/10.1088/1367-2630/17/2/023042 19. Oriti D (2018) Spacetime as a quantum many-body system. In: Angilella GGN, Amovilli C (eds) Many-body approaches at different scales: a tribute to norman H. March on the occasion

92

20. 21. 22. 23.

24. 25.

26. 27. 28.

29. 30. 31.

32. 33. 34. 35. 36.

37. 38. 39. 40. 41. 42.

4 Group Field Theory of his 90th birthday. Springer International Publishing, Cham, pp 365–379. ISBN 978-3-31972374-7. https://doi.org/10.1007/978-3-319-72374-7_29 Colafranceschi E, Oriti D (2021) Quantum gravity states, entanglement graphs and secondquantized tensor networks. JHEP 07:052. https://doi.org/10.1007/JHEP07(2021)052 Colafranceschi E, Chirco G, Oriti D (2021) Holographic maps from quantum gravity states as tensor networks. arXiv:2105.06454 Chirco G, Mele FM, Oriti D, Vitale P (2018) Fisher metric, geometric entanglement and spin networks. Phys Rev D97(4):046015. https://doi.org/10.1103/PhysRevD.97.046015 Chirco G, Goeßmann A, Oriti D, Zhang M (2020) Group field theory and holographic tensor networks: dynamical corrections to the Ryu-Takayanagi formula. Class Quant Grav 37(9):095011. https://doi.org/10.1088/1361-6382/ab7bb9 Chirco G, Oriti D, Zhang M (2018) Ryu-Takayanagi formula for symmetric random tensor networks. Phys Rev D97(12):126002. https://doi.org/10.1103/PhysRevD.97.126002 Chirco G, Oriti D, Zhang M (2018) Group field theory and tensor networks: towards a RyuTakayanagi formula in full quantum gravity. Class Quant Grav 35(11):115011. https://doi.org/ 10.1088/1361-6382/aabf55 Assanioussi M, Kotecha I (2020) Thermal representations in group field theory: squeezed vacua and quantum gravity condensates. JHEP 20:173. https://doi.org/10.1007/JHEP02(2020)173 Chirco G, Kotecha I, Oriti D (2019) Statistical equilibrium of tetrahedra from maximum entropy principle. Phys Rev D99(8):086011. https://doi.org/10.1103/PhysRevD.99.086011 Chirco G, Kotecha I (2019) Generalized Gibbs ensembles in discrete quantum gravity. In: Nielsen F, Barbaresco F (eds) Geometric science of information 2019. Lecture notes in computer science (LNCS). Springer, Cham Kotecha I, Oriti D (2018) Statistical equilibrium in quantum gravity: Gibbs states in group field theory. New J Phys 20(7):073009. https://doi.org/10.1088/1367-2630/aacbbd Kegeles A, Oriti D, Tomlin C (2018) Inequivalent coherent state representations in group field theory. Class Quant Grav 35(12):125011. https://doi.org/10.1088/1361-6382/aac39f Pithis AGA, Sakellariadou M (2019) Group field theory condensate cosmology: an appetizer. Universe 5(6). ISSN 2218-1997. https://doi.org/10.3390/universe5060147. https://www.mdpi. com/2218-1997/5/6/147 Oriti D (2017) The universe as a quantum gravity condensate. Comptes Rendus Physique 18:235–245. https://doi.org/10.1016/j.crhy.2017.02.003 Gielen S, Sindoni L (2016) Quantum cosmology from group field theory condensates: a review. SIGMA 12:082. https://doi.org/10.3842/SIGMA.2016.082 Gabbanelli L, De Bianchi S (2021) Cosmological implications of the hydrodynamical phase of group field theory. Gen Relativ Gravit 53(7):66. https://doi.org/10.1007/s10714-021-02833-z Li Y, Oriti D, Zhang M (2017) Group field theory for quantum gravity minimally coupled to a scalar field. Class Quant Grav 34(19):195001. https://doi.org/10.1088/1361-6382/aa85d2 Oriti D, Sindoni L, Wilson-Ewing E (2016) Emergent Friedmann dynamics with a quantum bounce from quantum gravity condensates. Class Quant Grav 33(22):224001. https://doi.org/ 10.1088/0264-9381/33/22/224001 Gielen S (2018) Group field theory and its cosmology in a matter reference frame. Universe 4(10):103. https://doi.org/10.3390/universe4100103 Gielen S, Polaczek A (2021) Hamiltonian group field theory with multiple scalar matter fields. Phys Rev D 103(8):086011. https://doi.org/10.1103/PhysRevD.103.086011 Rovelli C (1991) What is observable in classical and quantum gravity? Class Quant Grav 8:297–316. https://doi.org/10.1088/0264-9381/8/2/011 Rovelli C, Smolin L (1994) The physical hamiltonian in nonperturbative quantum gravity. Phys Rev Lett 72:446–449. https://doi.org/10.1103/PhysRevLett.72.446 Brown JD, Kuchar KV (1995) Dust as a standard of space and time in canonical quantum gravity. Phys Rev D51:5600–5629. https://doi.org/10.1103/PhysRevD.51.5600 Tambornino J (2012) Relational observables in gravity: a review. SIGMA 8:017. https://doi. org/10.3842/SIGMA.2012.017

References

93

43. Bojowald M, Hoehn PA, Tsobanjan A (2011) Effective approach to the problem of time: general features and examples. Phys Rev D 83:125023. https://doi.org/10.1103/PhysRevD.83.125023 44. Höhn PA, Vanrietvelde A (2020) How to switch between relational quantum clocks. New J Phys 22(12):123048. https://doi.org/10.1088/1367-2630/abd1ac 45. Höhn PA, Smith ARH, Lock MPE (2019) The trinity of relational quantum dynamics. https:// doi.org/10.1103/PhysRevD.104.066001 46. Hoehn PA, Smith ARH, Lock MPE (2021) Equivalence of approaches to relational quantum dynamics in relativistic settings. Front Phys 9:181. https://doi.org/10.3389/fphy.2021.587083 47. Assanioussi M, Kotecha I (2020) Thermal quantum gravity condensates in group field theory cosmology. Phys Rev D 102(4):044024. https://doi.org/10.1103/PhysRevD.102.044024 48. Marchetti L, Oriti D (2021) Effective relational cosmological dynamics from quantum gravity. JHEP 05:025. https://doi.org/10.1007/JHEP05(2021)025 49. Wilson-Ewing E (2019) A relational Hamiltonian for group field theory. Phys Rev D99(8):086017. https://doi.org/10.1103/PhysRevD.99.086017 50. Bratteli O, Robinson DW (1987) Operator algebras and quantum statistical mechanics. Vol 1: C* and W* algebras, symmetry groups, decomposition of states, 2nd edn. Springer, Berlin Heidelberg 51. Bratteli O, Robinson DW (1997) Operator algebras and quantum statistical mechanics. Vol 2: Equilibrium states, Models in quantum statistical mechanics, 2nd edn. Springer, Berlin Heidelberg 52. Fetter AL, Walecka JD (1971) Quantum theory of many-particle systems. International series in pure and applied physics. McGraw-Hill. https://books.google.de/books? id=Y1HwAAAAMAAJ 53. Mikovic AR (2001) Quantum field theory of spin networks. Class Quant Grav 18:2827–2850. https://doi.org/10.1088/0264-9381/18/14/313 54. Gielen S (2014) Quantum cosmology of (loop) quantum gravity condensates: an example. Class Quant Grav 31:155009. https://doi.org/10.1088/0264-9381/31/15/155009 55. Gielen S, Oriti D, Sindoni L (2013) Cosmology from group field theory formalism for quantum gravity. Phys Rev Lett 111(3):031301. https://doi.org/10.1103/PhysRevLett.111.031301 56. Gielen S, Oriti D, Sindoni L (2014) Homogeneous cosmologies as group field theory condensates. JHEP 06:013. https://doi.org/10.1007/JHEP06(2014)013 57. Barbieri A (1998) Quantum tetrahedra and simplicial spin networks. Nucl Phys B518:714–728. https://doi.org/10.1016/S0550-3213(98)00093-5 58. Baez JC, Barrett JW (1999) The Quantum tetrahedron in three-dimensions and fourdimensions. Adv Theor Math Phys 3:815–850. https://doi.org/10.4310/ATMP.1999.v3.n4.a3 59. Kowalski E (2014) An introduction to the representation theory of groups, vol 155. Graduate studies in mathematics. American Mathematical Society, Providence, RI. ISBN 978-1-47040966-1 60. Martin-Dussaud P (2019) A primer of group theory for loop quantum gravity and spin-foams. Gen Rel Grav 51(9):110. https://doi.org/10.1007/s10714-019-2583-5 61. Sewell GL (2002) Quantum mechanics and its emergent macrophysics. Princeton University Press 62. Strocchi F (2005) An introduction to the mathematical structure of quantum mechanics: a short course for mathematicians. Advanced series in mathematical physics. World Scientific. ISBN 9789812564313. https://books.google.de/books?id=ERcIVsPP48YC 63. Chaiken JM (1967) Finite-particle representations and states of the canonical commutation relations. Ann Phys 42(1):23–80. ISSN 0003-4916. https://doi.org/10.1016/0003-4916(67)901868. http://www.sciencedirect.com/science/article/pii/0003491667901868 64. Haag R (1992) Local quantum physics: fields, particles, algebras. Springer, texts and monographs in physics, Berlin, Germany 65. Fecko M (2006) Differential geometry and lie groups for physicists. Cambridge University Press. https://doi.org/10.1017/CBO9780511755590 66. Chirco G, Haggard HM, Rovelli C (2013) Coupling and thermal equilibrium in generalcovariant systems. Phys Rev D88:084027. https://doi.org/10.1103/PhysRevD.88.084027

94

4 Group Field Theory

67. Chirco G, Josset T (2016) Statistical mechanics of covariant systems with multi-fingered time. arXiv:1606.04444 68. Guedes C, Oriti D, Raasakka M (2013) Quantization maps, algebra representation and noncommutative Fourier transform for Lie groups. J Math Phys 54:083508. https://doi.org/10. 1063/1.4818638 69. Rovelli C, Smerlak M (2011) Thermal time and the Tolman-Ehrenfest effect: temperature as the ‘speed of time’. Class Quant Grav 28:075007. https://doi.org/10.1088/0264-9381/28/7/ 075007 ˇ (2019) Quantum mechanics and the covariance of 70. Giacomini F, Castro-Ruiz E, Brukner C physical laws in quantum reference frames. Nat Commun 10(1):494. https://doi.org/10.1038/ s41467-018-08155-0 71. Vanrietvelde A, Hoehn PA, Giacomini F, Castro-Ruiz E (2020) A change of perspective: switching quantum reference frames via a perspective-neutral framework. Quantum 4:225. ISSN 2521-327X. https://doi.org/10.22331/q-2020-01-27-225 72. de la Hamette A-C, Galley TD (2020) Quantum reference frames for general symmetry groups. Quantum 4:367. https://doi.org/10.22331/q-2020-11-30-367 73. Krumm M, Hoehn PA, Mueller MP (2020) Quantum reference frame transformations as symmetries and the paradox of the third particle. arXiv:2011.01951 74. Gambini R, Porto R, Pullin J (2004) A Relational solution to the problem of time in quantum mechanics and quantum gravity induces a fundamental mechanism for quantum decoherence. New J Phys 6:45. https://doi.org/10.1088/1367-2630/6/1/045 75. Rovelli C (1991) Quantum reference systems. Class Quantum Gravity 8(2):317–331. https:// doi.org/10.1088/0264-9381/8/2/012

Chapter 5

Thermal Group Field Theory

All the previously enumerated theorems are strict consequences of a single proposition: that stable equilibrium corresponds to the maximum of entropy. That proposition, in turn, follows from the more general one that in every natural process the sum of the entropies of all participating bodies is increased. Applied to thermal phenomena this law is the most general expression of the second law of the mechanical theory of heat ... —Max Planck1

Equipped with the many-body description of an arbitrarily large number of algebraic and combinatorial quanta of geometry from the previous sections, a statistical mechanics for them can formally be defined. Given a normal state ωρ , then the quantities ωρ [A] = Tr(ρ A) are the quantum statistical averages of operators A. If additionally, A is self-adjoint and has a structure that admits some physical interpretation, then ωρ [A] are ensemble averages of observables A. ωρ is a statistical mixture of quantum states encoding discrete gravitational and scalar matter degrees of freedom associated with the group field.2 Equilibrium statistical states are known to play an important role in describing macroscopic systems. Particularly, Gibbs thermal states are ubiquitous in physics, being utilised across the spectrum of fields, ranging from phenomenological thermodynamics, condensed matter physics, optics, tensor networks and quantum information, to gravitational horizon thermodynamics, AdS/CFT and quantum gravity. Even generic systems not at equilibrium may be modelled via the notion of local equilibrium, wherein various subsystems of the whole are locally at equilibrium, while 1

As cited in [1], p. 16. Group field theory, being a second quantisation of loop quantum gravity [2], then this reformulation of spin network degrees of freedom would allow us to define a statistical mechanics for them. 2

© The Author(s), under exclusive license to Springer Nature Switzerland AG 2022 I. Kotecha, On Generalised Statistical Equilibrium and Discrete Quantum Gravity, Springer Theses, https://doi.org/10.1007/978-3-030-90969-7_5

95

96

5 Thermal Group Field Theory

the whole system is not. Then, collective variables such as number and temperature densities, vary smoothly across these different patches, while having constant (equilibrium) values within a given subsystem. This basic idea underlies several techniques for coarse-graining in general, and as such displays again the usefulness of statistical equilibrium descriptions. Thus also in discrete quantum gravity, statistical equilibrium states would be of value, in ongoing efforts to get an emergent coarse-grained spacetime, based on techniques from finite-temperature quantum and statistical field theory. Also, equilibrium statistical mechanics provides a fundamental microscopic foundation for thermodynamics. Therefore, a statistical framework for some quantum gravitational degrees of freedom would also facilitate identification of thermodynamic variables with geometric interpretations originating in the underlying fundamental theory, to then make contact with studies in spacetime thermodynamics. Construction of several different examples of generalised Gibbs states in the present quantum gravity system is the focus of the first part of this chapter. Further, an increasing number of studies are hinting toward intimate links between geometry and entanglement. Spacetime is thought to be highly entangled, with quantum correlations in the underlying quantum gravitational system being crucial. Particularly in discrete approaches, a geometric phase of the universe is expected to emerge from a pre-geometric one via a phase transition, which must then also be highly entangled. The emergent phase must also encode a suitable notion of semiclassicality, for example by introducing coherent states. Moreover, fluctuations in relevant observables are expected to be important in the physics of a quantum spacetime, and thus must be included in the description of the system. In the second part of this chapter, we show how to construct quantum gravitational phases in group field theory (for now, kinematically) using techniques from thermofield dynamics, which display all these features, namely entanglement, coherence and statistical fluctuations in given observables. Finally, the ultimate goal of any theory of quantum gravity is to describe the known physics, while also providing novel falsifiable predictions on a measurable scale. An important arena in this respect is cosmology, with features such as singularity resolution and inflation representing crucial checkpoints for any viable model based on an underlying theory of quantum gravity. It is thus important for any candidate theory to find a suitable continuum and semi-classical regime within the full theory, in which standard cosmology can be approximated, up to effective corrections of quantum gravitational origin. In group field theory, such a regime has been suggested via a class of condensate phases of the system [3–6]. In the last part of this chapter, we consider a class of thermal condensates to derive an effective model of homogeneous and isotropic cosmology from non-interacting GFT dynamics, with corrections of quantum and statistical origins to the classical relational Friedmann equations. We begin in Sect. 5.1, with the construction of different examples of generalised Gibbs states associated with a variety of generators, utilising the many-body formalism introduced previously. In Sect. 5.1.1, we consider a class of positive, extensive operators in the GFT Fock representation induced by a degenerate vacuum. This class includes the special case of a volume operator. The corresponding states are defined using the maximum entropy principle. We show that these states naturally

5 Thermal Group Field Theory

97

admit Bose-Einstein condensation to the single-particle ground state of the generator (which corresponds to a low-spin phase in the spin representation). In Sect. 5.1.2, we consider the KMS condition for Gibbs states. We define equilibrium states with respect to momentum generators for translations on the group base manifold, both for internal translations corresponding to the C*-automorphisms in Sect. 5.1.2.1; and external translations corresponding to clock Hamiltonians after deparametrization in Sect. 5.1.2.2. In Sect. 5.1.3, we use the maximum entropy principle to consider a classical system of tetrahedra, fluctuating in terms of the geometric condition of closure in Sect. 5.1.3.1; and in terms of half-link gluing conditions in Sect. 5.1.3.2, leading to statistically fluctuating twisted geometries. In the next Sect. 5.2, we begin with an overview of the relevant essentials of the formalism of thermofield dynamics in Sect. 5.2.1. We use this formalism in the subsequent sections to present a systematic extension of group field theories, for constructing finite temperature equilibrium phases associated with generalised Gibbs states. Using the setup of bosonic group field theory coupled to a scalar matter field as presented in Sect. 4.1 above, we give a description for the zero temperature phase based on the degenerate vacuum in Sect. 5.2.2. Then focusing on positive extensive operators as generators for generalised Gibbs states, we construct their corresponding thermal vacua (thermofield double states), and the inequivalent phases generated by them, in Sect. 5.2.3. In Sect. 5.2.4 we introduce the class of coherent thermal states and give an overview of their useful properties. Finally in Sect. 5.3, we analyse a free GFT model for effective cosmology, based on the above construction of equilibrium thermal representations, and using coherent thermal states as candidates for thermal quantum gravitational condensates. In Sect. 5.3.1, we explicate the choice of the state, based on which we derive the GFT effective equations of motion in Sect. 5.3.2. In Sects. 5.3.3 and 5.3.4, we reformulate the effective dynamics in terms of relational clock functions, implemented as smearing functions along the φ direction of the base manifold. We show that this provides a suitable non-singular generalisation of the relational frame used in previous works in terms of the coordinate φ. We further derive the effective generalised Friedmann equations for flat homogeneous and isotropic cosmology in Sect. 5.3.5.1, recover the correct classical general relativistic limit in a late time regime in Sect. 5.3.5.2, and characterise the early time evolution through an assessment of singularity resolution and accelerated expansion in Sect. 5.3.5.3. We close with a discussion of some aspects surrounding the inclusion of interactions and its implications at the level of the effective thermal GFT models in Sect. 5.3.6.

5.1 Generalised Gibbs States In the study of bulk properties of a system of many discrete constituents, Gibbs states provide the simplest description  of the system, that of equilibrium. Generalised Gibbs states can be written as e− a βa Oa , where Oa are operators that are of interest in the situation at hand whose state averages Oa  are fixed, and βa are the

98

5 Thermal Group Field Theory

corresponding intensive parameters that characterise the equilibrium configuration (see Chap. 2 for details). Naturally, this leaves open the possibilities for the precise choice of the different observables. In fact, which ones are relevant in any given situation is an important part of the broader problem of investigating the statistical mechanics of quantum gravity for an emergent, thermodynamical spacetime with features compatible with semi-classical studies. In this section we present examples of generalised Gibbs states in discrete quantum gravity, by applying insights from discussions on generalised statistical equilibrium (as presented in Chap. 2) in group field theory (as presented in Chaps. 3 and 4).

5.1.1 Positive Extensive Operators 5.1.1.1

General

A particularly interesting class of operators for which the corresponding Gibbs states are well-defined, are positive extensive operators on H F of the form P=



λχ α aχ† α aχ α , λχ,  α ∈ R≥0

(5.1)

χ,  α

where labels χ , α denote the discrete basis introduced in Sect. 4.1.2. Notice that P is self-adjoint, by definition. Further P is an extensive operator, which means that it is proportional to the size of the system [7], i.e. the total number of quanta, or spin network nodes. Also, P is a one-body operator [7] on the Fock space, which means that its total action on any multi-particle state is additive, with irreducible contributions coming from individual actions on a single particle |χ,  α . Both these features are manifest in the fact that modes of P scale as the number density operator. A typical example of an extensive, one-body operator in a standard many-body quantum system is the total kinetic energy. In group field theory, extensive one-body operators are a second quantisation [7] of those loop quantum gravity operators which are diagonal in some intertwiner basis, such as the spatial volume operator [2, 8, 9]. Using the thermodynamical characterisation (Sect. 2.2.3), the corresponding Gibbs state is 1 −βP e . (5.2) ρβ = Zβ On a Fock space however, it is more natural to define states of the grand-canonical type, with fluctuating particle number, that is ρβ,μ =

1 Z β,μ

e−β(P−μN ) .

(5.3)

5.1 Generalised Gibbs States

99

These are self-adjoint, positive and trace-class (density) operators on H F , for 0 < β < ∞ and μ < min(λχ α ) for all χ and α . See Appendix 1 for details. Further, using the occupation number basis introduced in Sect. 4.1.2, the partition function can be evaluated to give,  1 (5.4) Z β,μ = 1 − e−β(λχ α −μ) χ,  α

as shown in Appendix 1. This is a grand-canonical state of quanta of the a-operators. Like in standard statistical mechanics, this state essentially describes a gas of these quanta of space with a changing total number in a given system. Notice that, for a constant μ, the number operator in (5.3) simply implements a shift in the spectrum of P by μ, thus allowing for an overall replacement λχ α − μ → λχ α , as will be done later in Sects. 5.2 and 5.3. It is evident that by construction, the parameter β controls the strength of statistical fluctuations in P, regardless of any other interpretations. Note however, that one can reasonably inquire about its geometric meaning, especially if the operator P, which is its thermodynamic conjugate, has a clear geometric interpretation. It would thus be interesting to investigate this aspect in a concrete example where the choice of the observable is adapted to a physical context, like cosmology (see for instance [10], or Sect. 5.3 in this thesis).

5.1.1.2

Spatial Volume

The volume observable plays a crucial role in quantum gravity. We recall that in loop quantum gravity there exist different proposals for a volume operator (see [8, 11–13] and references therein), but in each its spectral values are attached to the nodes of the labelled graphs. In other words, an elementary quantum of volume of space is assigned to a single node of a boundary graph. Since the GFT Fock space H F is the second quantisation of the spin network degrees of freedom [2], here a volume eigenvalue is associated to a quantum of the group field. Let us then consider a Gibbs state with respect to a volume operator V . As will be clear below, this is a special case of the states (5.3) defined above, with operator P now chosen to be the volume operator. We note that classical geometric observables, such as spatial volumes or areas of hypersurfaces, are not necessarily completely well-defined in a diffeomorphism invariant (background independent) context. This is because such quantities are at most diffeomorphism covariant, thus failing to represent a physical gauge-invariant observable. This open issue of understanding physical observables in general relativity, arises also within any background independent quantum gravity approach. Having said that, one could still construct mathematically well-defined quantum operators, formally associated with certain classical quantities in a given quantum framework, such as the volume of space. In this sense, one could still define operators

100

5 Thermal Group Field Theory

with a geometric interpretation in a background independent context, like in group field theory or loop quantum gravity. [14] In line with the original work reported in [9], here we choose to neglect the scalar matter degrees of freedom taking values in Rn , but it should be evident from Sect. 5.1.1.1 above that an extension to this case is directly possible. The main reasons for this choice are the following. First, in this example we are not particularly interested in matter degrees of freedom or any relational reference frames that they may define. For instance, in Sect. 5.3 in the context of cosmology, we will reinstate this dependence in order to define relational evolution. Second, the volume of a quantum of space is a geometric quantity expected to depend primarily on the group representation data χ . This is not to say that the volume of the corresponding emergent spacetime manifold would not depend on matter, which it of course does according to GR. This is also the standard choice made in LQG. With this in mind, the choice of independence of the volume observable from matter degrees of freedom should be viewed as a first step that is simple enough to investigate geometric properties of a theory of fundamental discrete constituents of spacetime. Volume Gibbs State Given a multi-particle boundary (graph) state, the total volume operator should basi and multiply this cally count the number of particles (nodes) n χ , in each mode χ, number by the volume eigenvalue vχ associated to a single particle (node) in that mode. It is thus an extensive, one-body operator, given by V =



vχ aχ† aχ .

(5.5)

χ

As long as the perspective of attaching a quantum of space to a graph node holds, a volume operator in a Fock space formulation of states of labelled graphs will always be of this form. This operator is diagonal in the occupation number basis (Sect. 4.1.2), with action        vχ n χ {n χ } . (5.6) V {n χ } = i

i

i

i

i

Keeping in mind our understanding of vχ as the volume of a quantum polyhedron with faces coloured by SU (2) representation data χ,  the following reasonable assumptions are made. First, the single-mode spectrum is chosen to be real and positive, i.e. (5.7) vχ ∈ R>0 for all χ . This implies that the spectrum of the total volume operator V is real and non-negative because it is simply a result of scaling vχ with occupation numbers n χ ∈ N≥0 . Therefore by construction, V is a positive, self-adjoint element of A F . Positivity ensures boundedness from below and therefore the existence of at least one ground state. Second, we assume uniqueness (or, non-degeneracy) of the singleparticle ground state, i.e. for v0 := min(vχ ), and V |χ0  = v0 |χ0 , we have

5.1 Generalised Gibbs States

101

vχ = v0 ⇔ χ = χ0 .

(5.8)

Naturally, the precise value of v0 depends on the specifics of the spectrum vχ , which in turn depends on the specific quantisation scheme used to define the operator. Our results are independent of these specifics. Notice that the uniqueness assumption would fail if the degenerate zero eigenvalue for vχ is included in the spectrum, because this could correspond to several different spin configurations. We stress however that non-degeneracy of the single-particle ground state |χ0  is assumed only for conceptual consistency in the upcoming scenario of Bose-Einstein condensation. In fact our technical results, particularly the definition of the state, will hold even without both these assumptions. This is clear from the discussions and proofs presented in Sect. 5.1.1.1 that are valid for spectrum λχ,  α ∈ R≥0 , thus including possibly degenerate zero eigenvalues. Then, the corresponding equilibrium state on H F is given by, ρ=

1 −β(V −μN ) e Z

(5.9)

with real parameters μ and 0 < β < ∞, and Z as given in (5.10). The details in Appendix 1 show that, for μ < v0 , the above ρ is a legitimate density operator. Let us pause to consider what it means to define such a Gibbs state, as generated by the volume operator. Referring back to the discussion in Sect. 2.2, specifically to the thermodynamical characterisation in a background independent setting, a state like (5.9) can be best understood as arising from the principle of maximisation of entropy, S = −ln ρ of the system, under the constraints I  = 1, V  = V and N  = N, without any need for a pre-defined flow. Parameters β and μ enter formally as Lagrange multipliers. From a purely statistical point of view, the corresponding physical picture, intuitively, would be that of a system in contact with a bath, which exchanges quantities corresponding to the operators V and N .3 The macroscopic description of the system is then given by the averages V and N, along with the intensive parameters β and μ4 which characterise the equilibrium phase. From a more general information-theoretic point of view, the system can be understood as being bi-partite, with the quanta (here, of the aχ field) in the state ρ describing the (sub) system of interest. In this case then, the full system can be understood as being in an entangled state, with a fixed large number of nodes. Then, partial tracing over the complement would give a (reduced) mixed state for the (sub) system of interest. We will discuss some of these aspects further in Sect. 5.2. A precise characterisation of the complementary subsystem (often interpreted as a thermal bath in statistical mechanics), boundary effects due to spin network links puncturing the boundary surface, consequences of entanglement across the boundary surface, and, 3

In the case at hand, exchange of particles inevitably leads to exchange of volume (and vice-versa), because the particles themselves carry the quanta of volume. In fact, μ is just a constant shift in the volume spectrum in this example. 4 Formally β and μ parametrise the class of Gibbs states (5.9). Presently no attempt is made to assign/require any additional interpretations to/of them.

102

5 Thermal Group Field Theory

the exact conditions and process for thermalisation of the subsystem to a Gibbs state are left to future work. Given our framework, defining a state like (5.9) is justified from both a quantum statistical and information-theoretic perspectives, as noted above. Now in the context of quantum gravity, such a state could be interesting to consider for the following reason. Instead of an arbitrary pure (spin network) state, a mixed state associated with geometric operators like volume or area would be expected to better describe the physical state of a region of space, wherein the corresponding macroscopic volumes or areas of regions are given by statistical averages, V ρ and Aρ ; and, such averages characterise, at least partially, the geometric macrostate (see for instance discussions in [15]). In other studies for example, a similar perspective is held with the aim of defining ‘geometric’ entropies, with respect to area measurements of boundary spin network links in [16], volume measurements of bulk links in [17], and in various LQG-inspired analyses of quantum black holes microstates [18, 19]. Within the framework described here, such geometrical entropies arise naturally as the information (von Neumann) entropy of a statistical state ρ associated with geometric observables. Condensation to Low-Spin Phase In addition to the link to macroscopic geometry that such states could provide, we show that they can lead to interesting phases purely as a result of the collective behaviour of the underlying quanta. Specifically, we show below that the volume Gibbs state as defined in (5.9) admits a condensed phase that is populated majorly by quanta in the lowest possible spin configuration χ0 . We also comment on a special sub-class of such condensates, the commonly encountered spin-1/2 phase, which is characterised by isotropic5 SU(2) spin network nodes and almost all links labelled by the same j = 1/2. As before, the occupation number basis of H F , being the eigenbasis of (5.5), can be used for computations. From Eq. (5.4), it is clear that the partition function in (5.9) is given by, Z=

  −β(v −μ)n    χi χi  {n χi } = {n χi } e

 {n χi }

i

χ

1 1−

e−β(vχ −μ)

.

(5.10)

This partition function can be observed to have the same form as that of a gas of free non-relativistic bosons in a Gibbs thermal state, which is defined in terms of the standard free Hamiltonian (total kinetic energy) operator [20]. In our case however, the simplicity of the state is not a statement about its underlying dynamics, or the result of some controlled approximation of some dynamics.6 For the simple case of the volume operator, unless our geometrical perspective of assigning a quantum of volume to a graph node changes, the corresponding operator will always be a onebody extensive operator (of the form (5.5)) in a Fock space formulation, and whose 5 6

All links incident on an isotropic node are labelled by the same spin. In fact, the present example is without the use of any specific dynamical ingredients.

5.1 Generalised Gibbs States

103

corresponding Gibbs partition function will be reminiscent of an ideal Bose gas. As is clear from Sect. 5.1.1.1, such a partition function will arise for any operator of the general form (5.1). Another example  is the kinetic part of a GFT action with a g )(− dI=1 g I + m 2 )ϕ( g ), which is used often in Laplacian term, SK = d g ϕ † ( the literature. This operator would naturally contribute to the system’s Hamiltonian, in cases when a suitable Legendre transform with respect to a chosen clock variable g ) are eigenstates of is possible [21]. Since the SU (2) Wigner expansion modes Dχ (   the Laplacian, we have, SK = χ (Aχ + m 2 )aχ† aχ , where Aχ = dI=1 j I ( j I + 1). Now, the average total number of particles in state (5.9) is,7 N = N ρ =

 χ

1 e+β(vχ −μ)

−1

.

(5.11)

It is clear that the dominant term in the above series corresponds to the ground state with the smallest eigenvalue v0 . Therefore, as μ → v0 , the average occupation number of the ground state, 1 N0 = +β(v −μ) (5.12) 0 e −1 diverges, and the system undergoes condensation. This results in a macroscopic occupation of the single-particle state |χ0  with volume v0 . A low-spin condensate phase thus arises naturally as a quantum statistical process in a system with a large number of quanta of geometry. Notice that this is analogous to standard Bose-Einstein condensation in a non-relativistic gas of free bosons [20]. The order parameter can now be directly seen as the non-zero expectation value of the group field operator, i.e.   (5.13) ψχ ( g )aχ ρ =  ψχ0 ( g )aχ0 + ψχ ( g )aχ ρ ϕ( g )ρ =  χ μ→v0



−→  ψχ0 ( g ) N0 cond

χ  =χ0

 = N0 ψχ0 ( g)

(5.14)

 ⊗N where |cond ≈ |N0 , 0, . . . = ψχ0 0 is the condensate state, and we have used 8 [20] wherein the ladder operators of the ground the Bogoliubov approximation √ state mode aχ0 ∼ N0 are of the order of the size of the condensed part. ψχ0 is the so-called condensate wavefunction.

7

In terms of the thermodynamic free energy F = V − μN ρ − β −1 S = − β1 ln Z , the average

F , like in standard thermodynamics. particle number is, N ρ = − ∂∂μ 8

An intuitive reasoning behind the Bogoliubov approximation is √ as follows. The action of say the annihilation operator on the condensate state is, aχ0 |N0 , . . . = N0 |N0 − 1, . . .. For a large √ enough system we have that N0  1, thus giving aχ0 |N0 , . . . ≈ N0 |N0 , . . .. Therefore the √ action of the ladder operators is simply to multiply the state by N0 . Hence, in this case, the √ operators can themselves be approximated by N0 I .

104

5 Thermal Group Field Theory

The single-particle state |χ0  characterising the condensate corresponds to a set of SU (2) spin labels, encoding the ground state data of the chosen quantum volume operator. A special class of such condensates is then for the choice of isotropic nodes of and a ground state corresponding to a minimum spin j0 = 1/2. Then, the above is a mechanism, which is rooted purely in the quantum statistical mechanics of group field quanta, for the emergence of a spin-1/2 phase. This configuration has been identified and used often as the relevant sector in LQG for loop quantum cosmology, and also in GFT condensate cosmology. Finally, we note that given the nice properties of the operator V that mimics the Hamiltonian of a system of non-interacting bosons in a box [20], the result that this system condenses to the single-particle ground state is not surprising in retrospect. Still, this simple example illustrates the potential of considering collective, statistical features that are inherent in the perspective that spacetime has a fundamental microstructure consisting of discrete quantum gravity degrees of freedom. It also illustrates the usefulness of the GFT perspective of a many-body discrete quantum spacetime, and the consequent reformulation of spin network degrees of freedom in a Fock space. For completeness, below we make a few specific remarks, in relation to similar results of obtaining spin-1/2 phases in the setting of GFT cosmology [22, 23]. These studies [22, 23] are carried out at a mean field level, in terms of an effective collective variable (condensate wavefunction σ ) of the underlying theory. While, our analysis as shown above [9] is directly at the level of the microscopic statistical theory, and not at an effective or approximate level. Further, the condensate state here is derived to  ⊗N be ψχ0 0 , and not assumed to be a coherent state from the start, which is a standard choice made in condensate cosmology (thus, also in [22, 23]). In fact, the starting point here is a maximally mixed state ρ. Moreover, the result here is more robust, with a low-spin phase arising as a universal model-independent feature of a class of thermal states characterised by extensive operators. Also, there is no restriction to isotropic nodes, unlike in the aforementioned studies in condensate cosmology. Finally, the low-spin phase is shown here to emerge already for only geometric degrees of freedom, without any coupling to scalar matter field. This is true also for the study in [23], which however, as pointed out above, is still at the mean field level and restricted to isotropic configurations, along with the choice of a specific class of models. We contrast this with the study in [22] wherein a spin-1/2 phase is shown to emerge from the particular wavefunction solution σ (φ), in an asymptotic regime of relational evolution φ → ±∞. Due to this crucial reliance on the inclusion of scalar matter field φ ∈ R in the GFT base manifold, it would seem that the consequent analysis is also restricted to models coupled to matter.

5.1 Generalised Gibbs States

105

5.1.2 Momentum Operators In this section, we turn our attention to the KMS condition and Gibbs states. As first examples in group field theory, we consider the relatively simple case of translation automorphisms along the base manifold, here G d × Rn . The automorphisms, and  and U ( their unitary representations U (φ) g ) on H F , have been defined earlier in Sect. 4.1.4. Let us begin with an important remark, which is independent of GFT, about the relation between Gibbs states and the KMS condition. In algebraic quantum statistical mechanics for finite-sized matter systems on spacetime, it is known that the unique normal KMS states, with respect to a given well-defined automorphism group, are Gibbs states (see Remark 1 in Appendix 2) [24–26]. Along similar lines in Appendix 2, we have shown that: given an algebraic system, described by a concrete C*-algebra A which is irreducible on a Hilbert space HA , equipped with a strongly continuous 1-parameter group of unitary transformations U (t) = eiGt , then the unique normal KMS state over A, with respect to U (t) at value β, is of the Gibbs form e−βG . It further follows (see the Corollary in Appendix 2) that this conclusion, of uniqueness of Gibbs states for a given automorphism group, also holds for an irreducible representation of an abstract C*-algebra. Since the above result relies solely on certain algebraic structures, we observe that it can also be applied to the GFT system at hand [9]. Since the Fock representation π F is irreducible on the GFT Weyl algebra A, we have that: given an automorphism group αt , with its strongly continuous unitary representation U (t) on H F , then the unique normal KMS state on π F (A), with respect to αt , is a Gibbs state characterised by the generator of the transformation. This extends naturally to the algebra B(H F ) of bounded linear operators on the GFT Fock space. Then, such states provide an explicit realisation of KMS states in the present quantum gravitational system.9

5.1.2.1

Internal Translations

Let G be a connected Lie group. Recall that any connected Lie group is pathconnected because as a smooth manifold it is locally-path-connected [29]. Thus any two points on G can be connected by a continuous curve.10 The natural curves to consider on any Lie group are the 1-parameter groups generated via the exponential map. Then, let (5.15) g X (t) = exp(t X ) , X ∈ G, ∀t ∈ R

9 Such states also amount to a concrete realisation of the thermal time hypothesis [27, 28], since they may be understood as defining implicitly a notion of time, when the corresponding automorphism implements physical evolution. However, much remains to be done in order to elucidate and analyse in detail their physical meaning and potential applications in discrete quantum gravity. 10 Notice that the groups relevant in GFT, namely S L(2, C), Spin(4), SU (2) and R, are all connected and simply connected, so that their direct product groups are also connected spaces.

106

5 Thermal Group Field Theory

be a 1-parameter subgroup in G, such that g X (0) = e ,

 dg X  =X dt t=0

(5.16)

where e ∈ G is the identity, and G = Te G is the Lie algebra of G. The generators of generic left translation flows, g X (t, g0 ) = et X g0 = L et X g0 , are the right-invariant vector fields, X. The set of all such vector fields is isomorphic to the Lie algebra by right translations Rg on G, that is {Rg∗ X | X ∈ G, g ∈ G} = {X(g)} .

(5.17)

g X : R → G, t → g X (t)

(5.18)

The map

is a continuous group homomorphism, preserving additivity of the reals, i.e. g X (t1 )g X (t2 ) = g X (t1 + t2 ) .

(5.19)

U : G → U(H)

(5.20)

Now, let be a strongly continuous unitary representation of G in a Hilbert space H, where U(H) is the group of unitary operators on H. Then, given the standard setup above [29], the map (5.21) U X := U ◦ g X : t → U (g X (t)) is a strongly continuous 1-parameter group of unitary operators in U(H). The group property is straightforward to see from, U (g X (t1 ))U (g X (t2 )) = U (g X (t1 )g X (t2 )) = U (g X (t1 + t2 ))

(5.22)

so that in terms of U X , we have the expected form, U X (t1 )U X (t2 ) = U X (t1 + t2 ) .

(5.23)

See Appendix 3 for proof of continuity [9]. Applying Stone’s theorem to this strongly continuous group of unitary operators leads to the existence of a self-adjoint (not necessarily bounded) generator G X defined on H, such that U X (t) = e−iG X t .

(5.24)

By construction, operator G X implements infinitesimal translations of quantum states in H, along the direction of the integral flow of X. It is thus understood as a momentum operator.

5.1 Generalised Gibbs States

107

Then, given the 1-parameter group of unitary transformations U X (t) in (5.24), equilibrium states on H are states that satisfy the KMS condition with respect to U X (t). Further, if G X has a discrete spectrumxi (e.g. on compact G or on a compact subspace of locally-compact G) such that i e−βxi converges, and if the algebra under consideration is irreducible on H, then as detailed in Appendix 2, this KMS state must be of the following Gibbs form, ρX =

1 −βG X e Z

(5.25)

where β is the periodicity in the flow parameter t. Notice that ρ X is characterised by both the periodicity β and the algebra vector X . Therefore, the corresponding notion of equilibrium has an intrinsic dependence on the curve used to define it. Further, the construction above holds independently of whether G is abelian, or not. The detailed Lie algebra structure determines whether the system retains its equilibrium properties on the entire G, or not. In other words, it determines whether the system is stable under arbitrary translation perturbations. The state ρ X , as defined by the curve g X (t), remains invariant under translations to anywhere on G if and only if G is abelian. Otherwise, the system is at equilibrium only along the curve which defines it. To see this, let us perturb a system at identity e in state ρ X , so that it leaves its defining trajectory g X (t), and reaches another point h ∈ G which is not on g X (t), i.e. h ∈ / {g X (t) | t ∈ R}. Since G is connected, any element of it can in general be written as a product of exponentials, i.e. h = exp Y1 . . . exp Yκ

(5.26)

for some finite κ ∈ N, and Y1 , . . . , Yκ ∈ G. Given the unitary representation U , left translation by h is implemented in the Hilbert space as, U (h) = U (exp Y1 ) . . . U (exp Yκ ) = exp(U∗ (Y1 )) . . . exp(U∗ (Yκ ))

(5.27)

where, U∗ is an anti-hermitian representation11 of G. This acts on the density operator as, U (h)−1 ρ X U (h) = e−U∗ (Yκ ) . . . e−U∗ (Y1 ) e−iβU∗ (X ) eU∗ (Y1 ) . . . eU∗ (Yκ )

(5.28)

For a finite-dimensional H, we recall that [29]: a representation D of a Lie group G on H, induces a unique representation D∗ of the Lie algebra Te G on H, such that D(exp X ) = exp(D∗ X ) (for any X ∈ Te G). In fact, D∗ is a differential map (or, push-forward) corresponding to the Lie group homomorphism D : G → G L(H), where G L(H) is the general linear group of all invertible linear operators on H. Then, for a unitary representation U , the derived representation U∗ is anti-hermitian, i.e. U∗ (X )† = −U∗ (X ), as expected. While for an infinite-dimensional complex Hilbert space H, there are more subtleties involved (as expected) but similar structures can be defined as long as U is a strongly continuous representation of G. Specifically, an anti-hermitian algebra representation U∗ is now defined on a dense subspace of H, the so-called Gårding domain [30]. We do not delve into these details further, mainly because we do not expect them to qualitatively change our result in Eq. (5.29), and also because these details are outside our scope presently. 11

108

5 Thermal Group Field Theory

where, G X = iU∗ (X ). For non-abelian G, clearly [X, Y ] = 0 for arbitrary X, Y ∈ G. Thus, we have (5.29) U (h)−1 ρ X U (h) = ρ X in the general, non-abelian case. While for abelian G, all Lie brackets are zero and equality will hold for arbitrary h, thus leaving the state invariant. So overall, the notion of equilibrium that we have defined here, with respect to translations on G, is curve-wise or direction-wise, with the “direction” being defined on each point of the manifold by the vector field X (uniquely associated with a given X ∈ G). For non-abelian G, an equilibrium state can be defined only along a particular direction.12 Applying this to the GFT system, we take: Hilbert space H to be the Fock space H F ; Lie group G to be, either Rn for internal scalar field translations, or G d for group left translations, both acting on the base manifold G d × Rn as detailed in Sects. 4.1.4.1 and 4.1.4.2 respectively; and, the strongly continuous unitary groups U (g) are those constructed in Sect. 4.1.4.3, which implement the translation automorphisms of the GFT Weyl algebra in H F . The form of the generators on the Fock space is,  X ϕ(  d g d φ ϕ † ( g , φ)L g , φ) (5.30) G X := i G d ×Rn

which is motivated from momentum operators for spatial translations in Fock representations of scalar field theories on spacetime. Here, X is the right-invariant vector field on G corresponding to the vector X ∈ G, and related to it by right translations as, X(g) = Rg∗ X (for g ∈ G); and, LX denotes the Lie derivative with respect to the vector field X. Then, equilibrium states for the GFT system are KMS states with respect to the automorphism group (5.24), where the generator is given by (5.30). Further, this state will be of the Gibbs form in (5.25), with generator (5.30) (which is suitably regularised when required, see below for an example). Equilibrium in Internal φ-Translations As a specific example of the momentum Gibbs states considered above, we now present those states that are in equilibrium with respect to flows on Rn part of the base space [9]. These are of particular interest from a physical perspective. First, we anticipate that in light of the interpretation of φ ≡ (φ1 , . . . , φa , . . . , φn ) ∈ Rn as n number of minimally coupled scalar fields [32, 33], the corresponding momenta that generate these internal translations are the scalar field momenta, so there is an immediate meaning to the variables. Second, and more important, the scalar values φ can be used as relational clocks, as in GFT cosmology [3–5, 33], thus their 12

This is also the case, for example, for the Unruh effect treated via the Bisognano-Wichmann construction [31]. In that case, the symmetry group G is the Lorentz group, acting on the base manifold which is a Rindler wedge of the Minkowski spacetime, and the KMS state of an accelerated observer depends on the specific trajectory generated by a 1-parameter flow of boosts (in say x 1 direction) taking the form k1 (t) = etak1 , where k1 is the boost generator, and acceleration a parametrises the strength of this boost. Another example from this thesis, is the classical Gibbs distribution with respect to the closure condition, in Sect. 5.1.3.1.

5.1 Generalised Gibbs States

109

translations can be related directly to dynamical evolution after deparametrization.  This is also the reason why we call the φ-translations here as being internal, to contrast with the case where the system is deparametrized with respect to one of these scalar fields, so that the resulting translations along this clock variable then become external to the system (thus defining relational evolution, see Sect. 4.2), and with respect to which then physical clock equilibrium can be defined (as done below in Sect. 5.1.2.2). The momentum of the clock scalar field defined within the reduced, deparametrized system then also gives the clock Hamiltonian. ∂ The basis of invariant vector fields on G = Rn is { ∂φ a } in cartesian coordinates a (φ ). These are generated by the set of basis vectors of the Lie algebra {E a }. The full set of invariant vector fields is then generated by linearity. For a generic tangent n n   λa E a , the corresponding invariant vector field is X = λa ∂a . Then vector, X = a=1

a=1

directly for the basis elements, generators (5.30) take the simple, familiar form,

∂   d g d φ ϕ † ( g , φ) ϕ( g , φ) ∂φ a  d p pa ϕ † (χ,  p) ϕ(χ , p) = (2π )n

G Ea = i

(5.31) (5.32)

χ

where pa ∈ R, and we have used the spin-momentum basis introduced in Sect. 4.1.2 for the second equality.13 Then, infinitesimal translations of the operators are generated in the expected way, e.g.  = i[G Ea , ϕ(  . g , φ) g , φ)] ∂φ a ϕ(

(5.33)

Notice that operators G Ea have a continuous and unbounded spectrum, as expected for any quantum mechanical momentum operator [30, 34, 35]. Then in order to consider well-defined quantities, we naturally need to consider suitable IR and UV regularisations. As per standard practice [34–36], let us: put our system in a finite box of size L n in Rn , with periodic boundary conditions, which results in a discrete Ma , where Ma ∈ Z; and, momentum spectrum,14 i.e. for each a, we have pa = 2π L put a high momentum cut-off, which renders the spectrum bounded from above, i.e. Ma0 = max( pa ). Denoting the resultant for each a, ∃ a finite Ma0 , such that pa0 = 2π L regularised operator by Pa , we have Pa =



pa ϕ † (χ , p) ϕ(χ , p)

(5.34)

χ,  p

which is diagonal in the occupation number basis, 13

We remark that the operators G Ea as constructed above are the same as those used in the GFT cosmology framework, and introduced in [33] for the case a = 1. 14 Recall that, from periodicity in momentum eigenfunctions, we have [34–36]: ei pφ = ei p(φ+L) ⇒ ei pL = 1 ⇒ p = 2π L M (where M ∈ Z).

110

5 Thermal Group Field Theory

        Pa {n χi , pi } = pa,i n χi , pi {n χi , pi }

(5.35)

i

where pa ∈ 2π Z, and pa,i is the ath component of the ith mode, i.e. pi = L ( p1 , . . . , pa , . . . , pn )i . Then, operators ρa =

1 −β(Pa −μN ) e Z

(5.36)

are generalised Gibbs states for −∞ < β < 0 and μ > pa0 . Here, β is negative because Pa is bounded from above (see the Remark in Appendix 1). Given these Pa along with the above ranges for β and μ, the proofs for boundedness, positivity and normalisation of ρa proceed in analogy with those in Appendix 1, to which we refer for details. Finally, we note that ρa as defined above, would naturally depend on the IR and UV cut-off parameters. Then, like in standard quantum statistical mechanics, one would consider the infinite volume and momentum limits to check the independence (or, specific dependences) of quantities of interest, e.g. correlation functions, on boundary conditions and regularisation. We leave further investigation of these states to future work.

5.1.2.2

Clock Evolution

The states defined above, generated by momenta (5.34), encode equilibrium with respect to internal φa -translations. These flows are structural, and so are the resultant equilibrium states, being devoid of any physical model-dependent information, in particular of a specific choice of dynamics. Below we present states, based on discussions in Sect. 4.2, that are at equilibrium with respect to a clock Hamiltonian encoding relational dynamics, wherein the φ-translations take on the role of an external clock evolution [9]. Recall from Sects. 2.1.2 and 4.2 that obtaining a good canonical structure in terms of a relational clock, i.e. deparametrization, amounts to the approximation deparam.

Cfull −→ C = pt + HN

(5.37)

for a constrained classical system (see Sect. 4.2.1). Then, the constraint surface post-deparametrization is  = ex |C=0 = R × can,N , which has the characteristic structure of foliation in clock time t ∈ R. Clock Hamiltonian is HN , which is a smooth function on can,N . Then, relational Gibbs distributions can in principle be defined on the canonical phase space can,N , taking the standard form ρcan =

1 −β HN e Z can

(5.38)

5.1 Generalised Gibbs States

111

where β ∈ R and HN are assumed to be such that Z can converges. This state is at equilibrium with respect to the flow Y HN that is parametrized by the clock time t. Equivalently, the state ρ=

1 −β Hphy e , π ∗ Hphy = HN Z

(5.39)

is a Gibbs state on the reduced, physical phase space phy,N , where π is the projection from constraint surface  to phy,N . This state is naturally at equilibrium with respect to the flow generated by Y Hphy . Notice that this flow on phy,N is determined by the Hamiltonian flow on , that is Y Hphy = −π∗ (∂t ), using π∗ (YC ) = 0 and YC = ∂t + Y HN . In the corresponding quantum system outlined in Sect. 4.2.2, formal constructions of the corresponding Gibbs density operators follow directly. A relational Gibbs ˆ

can ∝ e−β HN , which can further be state is a density operator on Hcan,N of the form ρ extended to the Fock space. Finally we remark that, heuristically we expect these relational states to be obtained from some reduction of the states defined in Sect. 5.1.2.1 above with respect to internal φ-translations, through the impositions of the dynamical constraint of the theory (i.e. being on-shell with respect to the given dynamics), and of the deparametrizing approximations on the same constraint. We leave detailed investigations of a rigorous link between these two classes of states to future work.

5.1.3 Constraint Functions In this section, we turn briefly to some explorations in a classical setting. From traditional statistical mechanics, we know that an important difference between canonical and microcanonical distributions over a phase space, is that the former includes also statistical fluctuations around a constant energy surface. In other words, a microcanonical distribution is characterised completely by a single energy shell, H = E, while a canonical distribution is characterised by a constant average energy, H  = E. Therefore, in a canonical (or a grand-canonical) state, the same amount of internal energy may be distributed over many more microstates. Further, canonical (and grand-canonical) states are often technically easier to handle, compared to the microcanonical one, to study physical properties of a system. Motivated by this, one might inquire if statistical distributions may be utilised to study the physics of a constrained system more conveniently, in an approximate or effective way, by considering a weaker constraint equation C = 0, instead of the exact one C = 0 that specifies the presymplectic constraint surface. Then, a generalised Gibbs distribution with respect to a finite set of scalar constraint functions {Ca }a=1,2,...,k on an extended phase space ex , would encode statistical fluctuations around the constraint surface. In this sense, the constraint information might be encoded partially or weakly in a statistical distribution that is defined on the full unconstrained extended state space.

112

5 Thermal Group Field Theory

This might be interesting to consider also because in a system with many degrees of freedom, observable averages correspond to statistical averages in generic mixed quantum states. However, in a constrained system it may be difficult to precisely find the physical state space, i.e. the space of all gauge-invariant states. In this case, we could consider instead states that satisfy the dynamical constraint only effectively, by fulfilling the weaker condition C = 0, instead of the exact one; and subsequently evaluate observable averages in this approximately physical state. Then, from the maximum entropy principle, one is naturally led to a state of the form (5.40) below. We say that a system satisfies a set of constraints weakly if Ca ρ = Ua , for some statistical state ρ on an extended phase space ex , and real constants Ua . Then by the thermodynamical characterisation (Sect. 2.2.3), the state ρ is given by ρ{βa } =

1 Z {βa }

e

−

k 

βa Ca

a=1

.

(5.40)

On the other hand, we say that a system satisfies a set of constraints strongly if Ca = Ua . This identifies the constraint submanifold  = ex |{Ca =Ua } ⊂ ex . From a statistical viewpoint, this same condition can be written in terms of a microcanonical density on ex , k 1  δ(Ca − Ua ) (5.41) ρ{Ua } = Z {Ua } a=1 where Z {Ua } = vol().15 Then for a fixed b, we have Cb = Ub ⇔ Cb ρ{Ua } =

ex

dλ Cb ρ{Ua } = Ub .

(5.42)

Therefore, the effective and exact impositions of constraints can be seen from a statistical perspective, as respectively either defining a Gibbs state of the form (5.40), or a microcanonical state of the form (5.41).16 In the following, we consider examples of the general form (5.40), in a system of classical tetrahedra.

15

Notice that the factorisation property of the state (equivalently, of the full partition function) is a consequence of the fact that we are considering a system of constraints each defined independently on ex . 16 Like in standard statistical mechanics, these two states, ρ {βa } and ρ{Ua } , are related by a Laplace transform between their respective partition functions, with their scalar component coefficients, βa and Ua , being the conjugate variables under the transform, i.e. (L Z U )(β) = Z˜ (β) ≡ Z β .

5.1 Generalised Gibbs States

5.1.3.1

113

Closure Condition

As a first example, we consider the relatively simple case of the closure constraint for a single classical tetrahedron17 [37, 38]. Recall that the symplectic phase space of intrinsic geometries of a convex tetrahedron is given by the 2-dim Kapovich-Millson phase space [39–41],  S4 = (X I ) ∈ su(2)

∗4

∼ =R

3×4

| ||X I || = A I ,

4 

 X I = 0 /SU (2)

(5.43)

I =1

where su(2)∗ is the dual space of the Lie algebra su(2); and, X I are the face normals of the four triangles in R3 , with fixed areas A I (for I = 1, 2, 3, 4). In particular, notice that the four co-vectors X I (and the surfaces associated to them, as orthogonal to each of them) close, that is 4  XI = 0 (5.44) I =1

thus giving a closed convex tetrahedron in R3 , modulo rotations. This is the closure constraint, which allows us to understand geometrically a set of 3d vectors as the normal vectors to the faces of a tetrahedron, and thus to fully capture its intrinsic geometry in terms of them (see Fig. 3.2) [39–42]. Now along the lines described above, we are interested in imposing this closure constraint effectively (on average) via a Gibbs distribution defined on an extended phase space. Then from a statistical perspective, we can interpret the strong fulfilment of closure (given above in (5.44)) as defining a microcanonical state with respect to this constraint, and therefore a generalised Gibbs state as encoding a weak fulfilment of the same constraint. Below we show that such a state can technically indeed be defined, but further investigation of any possible physical consequences of such a definition, in discrete gravity, is left to future work. Thus, let us remove the closure condition (5.44) from S4 , to define the phase space for an open tetrahedron, {A I } = {(X I ) ∈ su(2)∗4 ∼ = R3×4 | ||X I || = A I } ∼ = S2 × · · · × S2 A1

A4

(5.45) (5.46)

where each S 2A I is a 2-sphere with radius A I ∈ R>0 . This is the extended phase space of interest, with respect to the closure constraint. It is the space of sets of four oriented triangles in R3 , with face normals X I (and areas A I ) that are not constrained to close; and, SU (2) acts on it diagonally by rotation18 [42]. 17

The case of a classical d-polyhedron (Sect. 3.1) and its associated closure condition can be treated in a completely analogous manner to this one. 18 This is the adjoint action of SU (2) on  −1 {A I } : SU (2) × {A I }  g, (X I )  → (g X I g ) ∈ {A I } .

114

5 Thermal Group Field Theory

On the extended phase space {A I } , let us write the closure condition as a smooth map19 J : {A I } → su(2)∗ , defined by J (m) :=

4 

X I , ||X I || = A I

(5.47)

I =1

where m = (X 1 , . . . , X 4 ) ∈ {A I } denotes a point on the extended phase space manifold. We note that the symplectic reduction of {A I } with respect to the zero level set, J = 0, gives back the Kapovich-Millson phase space S4 = /SU (2), where  = J −1 (0) = {m ∈ {A I } | J (m) = 0} is the constraint surface [39, 42]. Then, a generalised Gibbs state with respect to closure for an open tetrahedron can be defined by: maximising the entropy functional (2.29) under normalisation (2.28), and the following su(2)∗ -valued constraint, J ρ =

{A I }

dλ ρ J = U

(5.48)

where ρ(m) is a statistical density on {A I } , and U ∈ su(2)∗ is a constant. Specifically, it can be defined by optimising the function (2.30), which in the present case takes the form, (5.49) L[ρ, β, κ] = − ln ρρ − β.(J ρ − U ) − κ(1ρ − 1) where now the Lagrange multiplier β ∈ su(2) for the constraint on J is algebravalued [44], and, b.x denotes an inner product between elements b ∈ su(2) of the algebra and x ∈ su(2)∗ of its dual. Then, δL =0 δρ

⇒

ρ = e−(β.J +1+κ)

(5.50)

which gives, ρβ =

1 −β·J e . Zβ

(5.51)

The equilibrium partition function is given by, Zβ = e

1+κ

= =

4  4π A I I =1

19

dλ e−β·J

(5.52)

{A I }

||β||

sinh(A I ||β||)

(5.53)

In more mathematically inclined literature on classical mechanics, this is known as a moment or momentum map; it is a generalisation of generators, of Hamiltonian actions on a phase space, to the case of generic non-abelian Lie groups [29, 43, 44]. In the present case, J generates a diagonal action of SU (2) on {A I } , i.e. simultaneous rotations of the spheres S 2A I [42, 44].

5.1 Generalised Gibbs States

115

for which, the details are provided in Appendix 4. Notice that, β.J : {A I } → R is a smooth real-valued function on the phase space, since the components βa and Ja (with a = 1, 2, 3) in any basis of the algebra or its dual, are real-valued, and scalar component functions Ja (m) are smooth. We can further write it as, (5.54) Jβ (m) = β.J (m) for m ∈ {A I } .20 Then, it is evident that Jβ is a modular Hamiltonian, i.e. Jβ = −d ln ρβ , with respect to which the state ρβ is at equilibrium (cf. discussions in Sect. 2.2.4). As expected, Jβ defines a vector field Xβ on {A I } via the equation, ω(Xβ ) = −d Jβ

(5.55)

where ω is the symplectic 2-form on {A I } . Xβ is the fundamental vector field corresponding to the vector β ∈ su(2). The state ρβ is at equilibrium with respect to translations along the integral curves of Xβ on the base manifold {A I } . In other words, ρβ encodes equilibrium with respect to the one-parameter flow characterised by β, which is a generalised vector-valued temperature [43, 44]. As encountered earlier in this thesis too, this is an expected feature of any equilibrium state associated with an action of a non-abelian Lie group (for instance, see Sect. 5.1.2).21 In fact, our construction here [37, 38] is an example of Souriau’s generalised Gibbs ensembles [43, 44] in a simplicial geometric context, associated with a Lie group (diagonal SU (2)) action for a first class (closure) constraint. Applications of the many results and insights from Souriau’s generalisation, and the corresponding Lie group extension of thermodynamics [43–46], in the present simplicial geometric setting are left to future work.

5.1.3.2

Gluing Conditions

We now turn to a system of many classical closed tetrahedra, and consider gluing conditions which constraint a set of disconnected tetrahedra to form an extended simplicial complex [37, 47]. The main motivation behind this consideration is the group field theory approach, which advocates for a many-body treatment of building blocks of spacetime, as we have seen repeatedly in this thesis. From this perspective, statistical distributions may naturally give rise to discrete quantum gravity partition functions, with the dynamical information being encoded in the statistical weight (cf. Sect. 3.4). Here, we consider statistical weights characterised by gluing constraints on the SU (2) data. The resulting distribution would then be a superposition of simplicial Jβ is the so-called comomentum map, associated with the momentum map J , for any β ∈ su(2) [44]. 21 Another example is the well-known case of accelerated trajectories on Minkowski spacetime, where thermal equilibrium is established along Rindler orbits defined by the boost isometry, where β encodes the strength of acceleration and defines the Unruh temperature. 20

116

5 Thermal Group Field Theory

Fig. 5.1 Gluing of adjacent faces in neighbouring tetrahedra via constraints on holonomy-flux variables. [37]

XmI

D

XnJ n

m

complexes, admitting a notion of a certain type of discrete geometry, on average. We note that our treatment below is formal. More work remains to be done for a complete understanding of the resulting distributions, including normalisability and further consequences in discrete quantum gravity. In the following, the key ingredient is a set of gluing conditions on the state space of many disconnected tetrahedra. As we will see, the same gluing process can be encoded in terms of dual graphs, which is the 1-skeleton of the cellular complex (dual to the simplicial complex) of interest. The geometry of the initial set of tetrahedra, as well as of the resulting simplicial complex, is captured by the T ∗ SU (2) data introduced earlier in Sect. 3.1. We will perform our construction in terms of these data first. A more refined characterisation of the same notion of discrete geometry can be obtained in terms of the so-called twisted geometry decomposition [48, 49], which we will connect with at a second stage, to suggest further research directions based on our construction. Setup Let γ denote an oriented, 4-valent closed graph with L number of oriented links and N number of nodes. Each link  is dressed with T ∗ SU (2) ∼ = SU (2) × su(2)∗  (g , X  ) data, with variables satisfying invariance under diagonal SU (2) action at each node n, thus satisfying closure. γ is dual to a simplicial complex γ ∗ , with links dual to triangular faces  and nodes dual to tetrahedra n. The source and target nodes (tetrahedra) sharing a directed link (face)  are denoted by s() and t () respectively. A state {(g , X  )}γ on the graph γ is then an element of γ = T ∗ SU (2) L //SU (2) N , where the double quotient denotes symplectic reduction of T ∗ SU (2) L with respect to closure at all nodes. Such configurations admit a notion of discrete geometry called twisted geometries [48, 49], the details of which we will return to below. The geometry so-defined is potentially pathological, in the sense that the resulting simplicial complex may not be fully specified in terms of metric data, that is its associated edge lengths, as a Regge geometry [50, 51] would be. For our purposes, though, this characterisation suffices to show how a statistical state can formally be constructed based on encoding gluing, and possibly other constraints, on the initially disconnected tetrahedra. To understand better the gluing process, and the corresponding constraints, let us begin with a single closed classical tetrahedron n. Recall that its state space is given

5.1 Generalised Gibbs States Fig. 5.2 a Dipole gluing in a system of two tetrahedra. b Combinatorics of the dipole gluing. [37]

117

(Xm4 , Xn4 )

(a)

(Xm1 , Xn1 ) D

n

m

(Xm3 , Xn3 ) (Xm2 , Xn2 )

(b)

by,

m

 = T ∗ (SU (2)4 /SU (2))

n

(5.56)

as in Eq. (3.3). As discussed before in Sect. 3.1,  is the space where 3d rotations have not been factorised out. This essentially means that each such tetrahedron is equipped with an arbitrary (orthonormal) reference frame determining its overall orientation in its R3 embedding. In the holonomy-flux representation, the four triangular faces |n of a given tetrahedron n, are labelled by the four pairs (g , X  ). In the dual picture, we have a single open graph node n, with four half-links |n incident on it and each labelled by (g , X  ). Each half-link is bounded by two nodes, one of which is the central node n, common to all four , and the other is a bounding bivalent node. This is a 4-patch labelled with T ∗ (SU (2)) data (see Sect. 3.1). For example: in Fig. 5.2a, the dipole graph is composed of two such 4-valent nodes, with the bivalent nodes shown as green squares; and in Fig. 5.3, the 4-simplex graph is composed of five 4-valent nodes, with the various bivalent nodes shown as green squares. Each  is oriented outward (by choice of convention) from the common 4-valent node n, which then is the source node for all four half-links. Then in the holonomy-flux parametrisation, each half-link  is labelled by (g , X  ). Let us denote the I th half-link belonging to an open node n by (n I ), where I = 1, 2, 3, 4. Equivalently, (n I ) denotes the I th face of tetrahedron n. Two tetrahedra n and m are said to be neighbours (see Fig. 5.1) if at least one pair of faces, (n I ) and (m J ), are adjacent, i.e. the variables assigned to the two faces satisfy the following constraints, (5.57) g(n I ) g(m J ) = e , X (n I ) + X (m J ) = 0 . A given classical state associated to the connected graph γ can then be understood as a result of imposing the constraints (5.57) on pairs of half-links (or, faces) in a system of N open nodes (or, disconnected tetrahedra). That is, γ is a result of imposing

118

5 Thermal Group Field Theory

Fig. 5.3 Resultant 4-simplex from combinatorial gluing between faces of five tetrahedra. Equivalently, the complete graph on five 4-valent nodes. [37]

n

(Xm1 , Xn1 )

o

m

q

p

L number each of SU (2)-valued and su(2)∗ -valued constraints, which we denote by C and D respectively. This is a total 6L number of R-valued constraint component functions {C,a , D,a }γ , for  = 1, 2, . . . , L and a = 1, 2, 3. For instance, creation of a full link  = (n I, m J ) involves matching the fluxes, component-wise, a a by imposing the three constraints D,a = X (n I ) + X (m J ) = 0, as well as restricting the conjugate parallel transports to satisfy C,a = (g(n I ) g(m J ) )a − ea = 0. Naturally the final combinatorics of γ is determined by which half-links are glued pairwise, which is encoded in which specific pairs of such constraints are imposed on the initial data. As an example, consider the dipole graph in Fig. 5.2. This can be understood as imposing constraints on pairs of half-links of two open 4-valent nodes. Here L = 4, thus we have at hand four constraints D on flux variables, X (11) + X (21) = 0 , X (13) + X (23) = 0 ,

X (12) + X (22) = 0 , X (14) + X (24) = 0 .

(5.58)

This corresponds to a set of 3 × 4 component constraint equations D,a = 0. Similarly for holonomy variables. As another example, consider a 4-simplex graph made of five 4-valent nodes as shown in Fig. 5.3. The combinatorics is encoded in the choice of pairs of half links that are glued. Here L = 10, corresponding to ten constraints D on the flux variables,

5.1 Generalised Gibbs States

119

X (12) + X (21) = 0 ,

X (13) + X (31) = 0 ,

X (14) + X (41) = 0 , X (23) + X (32) = 0 , X (25) + X (52) = 0 ,

X (15) + X (51) = 0 , X (24) + X (42) = 0 , X (34) + X (43) = 0 ,

X (35) + X (53) = 0 ,

X (45) + X (54) = 0 .

(5.59)

As before, this corresponds to 30 component equations for the flux variables, and another 30 for holonomies. Statistical Mixtures When the above constraints are satisfied exactly, that is {C,a = 0 , D,a = 0}γ for all , a, then this system of N tetrahedra admits a twisted geometric interpretation based on the resultant simplicial complex. But as discussed previously, there is a way of imposing these constraints only on average, that is {C,a ρ = 0 , D,a ρ = 0}γ . This manner of imposing effective constraints and maximising the Shannon entropy results in a generalised Gibbs state, parametrised by 6L number of generalised temperatures, ρ{γ ,α,β} ∝ e

−

L  3 

(α,a C,a +β,a D,a )

=1 a=1

≡ e−G γ (α,β)

(5.60)

where α, β ∈ R3L are multivariable inverse temperatures. The creation of a full link  is thus associated with two R3 -valued temperatures, α ≡ {α,a }a=1,2,3 and β ≡ {β,a }a=1,2,3 . Notice that the constraints {C,a , D,a }γ are smooth functions on  N =  ×N , and thus ρ{γ ,α,β} is a state of the N particle system. For instance, for the 4-valent dipole graph of Fig. 5.2 with flux constraints (5.58) and the corresponding holonomy ones, we have G dip (α, β) =

4  3 

α,a C,a (g(1) , g(2) ) + β,a D,a (X (1) , X (2) ) .

(5.61)

=1 a=1

We could further consider the case of assigning a single temperature for all three components a. Then, one pair of R-valued parameters, α and β , controls each link , instead of three pairs. We would thus get, ρ{γ ,α,β} ∝ e

−

L  =1

α C +β D

(5.62)

  where α, β ∈ R L , C = a C,a and D = a D,a [37]. Making such different choices is a non-trivial move (cf. discussions in Sect. 2.3.2); notice that {C,a = 0, D,a = 0}γ ⇒ {C = 0, D = 0}γ but the converse is not true. Latter is thus a weaker condition than the former. States (5.60) and (5.62) correspond to these two sets of conditions respectively, associated with the constraints, s1 = {C,a  =

120

5 Thermal Group Field Theory

0, D,a  = 0}γ and s2 = {C  = 0, D  = 0}γ , in the entropy maximisation procedure. If we were further to extract a single common temperature, say βγ , then this would correspond to a set with a single constraint, s3 = {G γ  = 0}γ (cf. discussions in Sect. 2.3.2). Being associated with a sum of all constraints, s3 is in turn weaker than both s1 and s2 . Then, the state with respect to s3 is naturally of the form ρβγ ∝ e−βγ G γ . Notice that, in the weaker cases s2 and s3 , the corresponding microcanonical states cannot be understood as giving back a state in γ , i.e. as giving a twisted geometry (unlike s1 ). This is because making γ requires imposing {C,a = 0, D,a = 0}γ (which is a microcanonical state of s1 ), and not either of the two weaker conditions. A state such as (5.60) is a statistical mixture of configurations where the ones which are glued with the combinatorics of γ , and thus admit a discrete geometric interpretation, are weighted exponentially more than those which are not. In this sense, such a state illustrates a statistically approximate notion of discrete (here, twisted) geometry. Notice that states like (5.62) and ρβγ would encode an even weaker notion of statistically fluctuating (approximate) geometries, even if that, because in general even those configurations satisfying {C = 0, D = 0} or G γ = 0 exactly would not necessarily correspond to a graph in γ . We can further generalise the above to include different ‘interaction’ terms, each corresponding to a given combinatorial pattern of gluings associated with a different graph γ . Let us first take into account all possible graphs {γ } N with a fixed number of nodes N . To each γ in this set corresponds a gluing G γ (α, β) as a function of several temperatures, which control the fluctuations in the internal structure of the graph γ . We can then think of a statistical mixture of the different graphs, each being represented by its corresponding gluing function G γ and weighted by coupling parameters λγ . Such a Gibbs distribution can be formally written as, 

− 1 e {γ } N ρN = Z N (λγ , α, β)

1 ksym

λγ G γ (α,β)

(5.63)

where ksym factors out any repetitions due to underlying symmetries, say due to graph automorphisms [37]. The choice of the set {γ } N is a model-building choice, analogous to choosing different interaction terms in the Hamiltonian of a standard many-body system. This can heuristically be generalised further to a superposition of such internally fluctuating twisted geometries for an N particle system, but now including contributions from distinct graphs, each composed of in general a variable number of nodes M. In line with analogous expressions in standard many-body theory, a state of this kind can formally be written as, M max



− 1 e M=2 {γ } M ρN = Z N (Mmax , λγ , α, β)

1 ksym

λγ

N  i 1 =··· =i M =1

G γ (gi1 , X i1 ,...,gi M , X i M ;α,β)

(5.64)

5.1 Generalised Gibbs States

121

where i is the particle index, and Mmax ≤ N [47]. The value of Mmax and the set {γ } M for a fixed M are model-building choices. The first sum over M includes contributions from all admissible (depending on the model, determined by Mmax ) different Mparticle subgroups of the full N particle system, with the gluing combinatorics of the different boundary graphs with M nodes. The second sum is a sum over all admissible boundary graphs γ , with a given fixed number of nodes M. And, the third sum takes into account all M-particle subgroup gluings (according to a given fixed γ ) of the full N particle system. We note that the state (5.64) is a further generalisation of the state (5.63) above, specifically the latter is a special case of the former for the case of a single term M = Mmax = N in the first sum. Let us consider a simple example, to understand better the definition of (5.64). Let the total number of particles be N = 3; and, the model be defined by a single, two-particle interaction, i.e. Mmax = 2. Let this interaction be characterised by a single 2-particle graph, say a dipole graph, i.e. the set of admissible graphs is {γdip }. Then, in the exponent: the first two sums contribute with a single term each; and, the last sum is 3 3  

G dip ( gi1 , X i1 , gi2 , X i2 ; α, β)

(5.65)

i 1 =1 i 2 =i 1 =1

g1 , X 1 , g2 , X 2 ; α, β) ≡ G dip (α, β) as given in Eq. (5.61) above. This where, G dip ( sum consists of six terms in total, which reduce to three for indistinguishable particles. This corresponds to the three possible pairings of the total N = 3 particles, i.e. the three number of 2-particle subgroups in a system with total 3 particles; and, each 2-particle subgroup interacts by G dip . Finally, allowing for the system size N to vary, we get a grand-canonical state, Z (μ, Mmax , λγ , α, β) =



eμN Z N (Mmax , λγ , α, β)

(5.66)

N ≥0

where μ is the Lagrange parameter for N , and Z N is the canonical partition function for a finite number of tetrahedra, but including different graph contributions given by the state (5.64). The resultant set of parameters {μ, Mmax , λγ , α, β} are thus directly derived from the underlying microscopic model, as should be the case in any statistical consideration. Discussion Now that we have discussed states for many classical tetrahedra, involving gluing constraints that impose a discrete geometric interpretation, we conclude with a brief discussion of some model-building strategies in the context of simplicial gravity. Any such strategy would have to be based on a clear understanding of how simplicial geometry is encoded in the data that is used. For instance, in the case of holonomy-flux geometries discussed above, the simplicial geometric content is precisely that of classical twisted geometries [48, 49]. In other words, the holonomy-flux variables admit an equivalent parametrisation in terms of twisted geometries vari-

122

5 Thermal Group Field Theory

ables. This relies on the fact that the link space T ∗ SU (2) can be decomposed as S 2 × S 2 × T ∗ S 1  (Ns() , Nt () , A , ξ ), modulo null orbits of the latter, and up to a Z2 symmetry. The variables are related by the following canonical transformations, g = ns eξ τ3 n−1 t ,

X = Ans τ3 n−1 t

(5.67)

where ns,t ∈ SU (2) are those elements which in the adjoint representation R rotate 3 vectors Ns,t respectively. That is Ns,t = R(ns,t ).z, the vector z ≡ (0, 0, 1) to give R 3 −1 or equivalently ns,t τ3 ns,t = a=1 Nas,t τa respectively for s and t, where τa = − 2i σa are generators of su(2), with Pauli matrices σa . Vectors Ns() and Nt () are unit normals to the face  as seen from two arbitrary, different orthonormal reference frames attached to s() and t () respectively. A is the area of , and ξ is an angle which encodes (partial22 ) extrinsic curvature information. So, a closed twisted geometry configuration supported on graph γ is: an element of  T ∗ S 1 n S4 , where S4 is the Kapovich-Millson phase space of a tetrahedron given a set of face areas; each link of γ is labelled with (A , ξ ); and each node of γ is labelled with four area normals (in a given reference frame) that satisfy closure [48, 49]. A twisted geometry is in general discontinuous across the faces, and so is the one described in terms of holonomy-flux variables, because both contain the same information. Face area A of a shared triangle is the same as seen from tetrahedron s() or t () on either side, but the edge lengths when approaching from either side may differ in general [48]. That is, the shape of the triangle , as seen from the two tetrahedra sharing it, is not constrained to match. If additional shape-matching conditions [52] were satisfied, then we would instead have a proper Regge (metric) geometry on γ ∗ , which is then a subclass of twisted geometries. These shape-matching conditions can be related to the so-called simplicity constraints, which are central in all model building strategies in the context of spin foam models, and whose effect is exactly to enforce geometricity (in the sense of metric and tetrad geometry) on discrete data of the holonomy-flux type, characterising (continuum and discrete) topological BF theories. The gluing constraints in Eq. (5.57), take the form of the following constraints in twisted geometry variables, A(n I ) − A(m J ) = 0 , ξ(n I ) + ξ(m J ) = 0 , Ns(n I ) − Nt (m J ) = 0 , Nt (n I ) − Ns(m J ) = 0 .

(5.68)

The result is naturally the same as in the holonomy-flux case: half-links (n I ) and (m J ) which satisfy the above set of six component constraint functions (in either of

The remaining two degrees of freedom of extrinsic curvature are encoded in the normals Ns() and Nt () [48]. For instance, in the subclass of Regge geometries, ξ is proportional to the modulus of the extrinsic curvature [49]. 22

5.1 Generalised Gibbs States

123

the parametrisations) are glued23 to form a single link  ≡ (n I, m J ). Equivalently, the two faces of the initially disconnected tetrahedra are now adjacent. The more refined parametrisation used in the twisted geometry language would allow for a model-building strategy leading, for example, to statistical states in which only some of the gluing conditions are imposed strongly, while others are imposed on average. In the same spirit of achieving greater geometrical significance of the statistical state that one ends up with, this construction scheme can be applied with additional constraints, beyond the gluing ones that we illustrated above. For instance, starting with the space of twisted geometries on a given simplicial complex dual to γ , one could consider imposing (on average) also shape-matching constraints, or simplicity constraints, to encode an approximate notion of a Regge geometry using a Gibbs statistical state. This would be the statistical counterpart of the construction of spin foam models, i.e. discrete gravity path integrals in representation theoretic variables [53–55], based on the formulation of gravity as a constrained BF theory. These lines of investigations are left to future work. Lastly, we remark that the quantum counterparts of the above states can formally be defined on H F , and the general discussion above is applicable [2, 37]. The basic ingredient of gluing is again to define face sharing conditions. For instance, the classical constraints of Eq. (5.57) can be implemented by group averaging of wavefunctions [2],  −1 }) = dh (n I,m J ) ψ({g(n I ) h (n I,m J ) , g(m J ) h (n I,m J ) }) γ ({g(n I ) g(m J) (n I,m J )|γ

SU (2)

(5.69) where ψ ∈ H N is a wavefunction for a system of generically disconnected N tetrahedra. So, a wavefunction defined over full links (n I, m J ) of a graph γ is a result of averaging over half-links (n I ) and (m J ) by SU (2) elements h (n I,m J ) . The same can also be implemented in terms of fluxes X , using a non-commutative Fourier transform between the holonomy and flux variables [2, 56, 57].

5.2 Thermofield Doubles, Thermal Representations and Condensates Quantum gravitational phases that display features like entanglement, coherence and observable statistical fluctuations are important in the study of semi-classical and effective continuum descriptions of quantum spacetime, especially in physical settings like cosmology and holes. In this section, we construct entangled,  black  thermofield double states ρ , associated with a generalised Gibbs state ρ. These states naturally encode statistical fluctuations with respect to the given observables 23

Gluing the two half-links is essentially superposing one over the other in terms of aligning their respective reference frames. This is evident from the constraints for the normal vectors N which superposes the target node of one half-link on the source node of the other, and vice-versa.

124

5 Thermal Group Field Theory

of interest, characterising ρ. We further construct their corresponding inequivalent representations. Subsequently,   we introduce a family of thermal condensates built upon the thermal vacua ρ , as coherent configurations of the underlying quanta [14].

5.2.1 Preliminaries: Thermofield Dynamics Thermofield dynamics (TFD) is an operator framework for finite temperature quantum field theory [58–62]. One of its main advantages lies in the fact that its formulation parallels that of zero temperature quantum field theory. Thus powerful tools of the temperature-independent setup can be translated to the thermal case, including perturbative Feynman diagrammatic techniques, symmetry breaking analyses, and for what concerns us here, Fock space techniques. TFD has been applied in various fields such as superconductivity, quantum optics, and string theory. The core idea of the TFD formalism is to represent statistical ensemble averages as temperature-dependent vacuum expectation values. That is, given a system described by a Hilbert   space h and an algebra of observables Ah on h, one looks for a vector state ρ (thermal vacuum) in a Hilbert space H, corresponding to a density operator ρ on h, such that the following condition holds for all observables A of the system,    Trh (ρ Ah ) = ρ  AH ρ H

(5.70)

where the subscript h or H denotes a suitable representation of the operator in the respective Hilbert spaces. Here, we are mainly concerned with statistical equilibrium, −βOh as discussed in the previous thus with density operators of the Gibbs form  e  sections. Further, notice that the vector state ρ encodes the same information as the density operator ρ, as reflected in Eq. (5.70) holding for the full algebra. Thus, like in standard treatments   of systems in a state ρ, statistical fluctuations in the corresponding state ρ can be investigated for instance in terms of variances of relevant observables in this state. A vector state satisfying Eq. (5.70) can only be defined in an extended Hilbert space, by supplementing the original degrees of freedom with the so-called tilde conjugate degrees of freedom [58]. Importantly, this doubling, or in general an enlargement of the space of the relevant degrees of freedom, is a characteristic feature of finite temperature description of physical systems. This was discovered also in algebraic quantum field theory for equilibrium statistical mechanics [63]. In fact, Eq. (5.70) is strongly reminiscent of the construction of a GNS representation   induced by an algebraic statistical state [24, 26, 64, 65], with the vector state ρ being the cyclic vacuum of a thermal representation. These intuitions have indeed led to tangible relations between the two formalisms, with the tilde degrees of freedom of TFD being understood as those of the conjugate representation of KMS theory in the algebraic framework [59, 62, 66–68].

5.2 Thermofield Doubles, Thermal Representations and Condensates

125

As we have noticed previously, these structures are also encountered commonly in quantum information theory [69], which in turn is utilised heavily in various areas  of modern theoretical physics, like holography. Specifically, constructing a state ρ is simply a purification of ρ. A prime example of a vector state is the thermofield double state, which is the purification of a Gibbs density operator. These states are used extensively in studies probing connections between geometry, entanglement, and more recently, complexity [70, 71]. For instance in AdS/CFT, this state is important because an eternal AdS black hole bulk is dual to a thermofield double in the boundary quantum theory [72]. We now review the basics of the TFD formalism [58–62], based on which we will later carry out our construction of thermofield doubles and their associated inequivalent representations in GFT. Here we consider a simple example of an oscillator, which will be extended to a field theory setup directly for GFTs in the subsequent sections. Consider a single bosonic oscillator, described by ladder operators a and a † , satisfying the commutation algebra, [a, a † ] = 1 , [a, a] = [a † , a † ] = 0

(5.71)

with the a-particle vacuum being specified by a |0 = 0 .

(5.72)

A Fock space h is generated by actions of polynomial functions of the ladder operators on |0. Thermal effects are then encoded in density operators defined on h. In particular, an equilibrium state at inverse temperature β is a Gibbs state, ρβ =

1 −β H e Z

(5.73)

where H is a Hamiltonian operator on h, possibly of grand-canonical type. But as discussed in Chap. 2 and Sect. 5.1 above, in the context of background independent systems one may work (at least formally) with other observables in place of H . This system is extended by including tilde degrees of freedom, spanning a Hilbert space h˜ generated by the ladder operators a˜ and a˜ † satisfying the same bosonic algebra, ˜ a] ˜ = [a˜ † , a˜ † ] = 0 (5.74) [a, ˜ a˜ † ] = 1 , [a, acting on the tilde-vacuum given by, ˜ = 0. a| ˜ 0 All tilde and non-tilde degrees of freedom commute with each other, that is

(5.75)

126

5 Thermal Group Field Theory

[a, a] ˜ = [a, a˜ † ] = [a † , a] ˜ = [a † , a˜ † ] = 0 .

(5.76)

The Hilbert space h˜ is conjugate to the original one via the following tilde conjugation rules of thermofield dynamics (or equivalently, via the action of the modular ˜ = A, ˜ (A† )˜ = A˜ † , ( A)˜ conjugation operator of KMS theory [66]): (AB)˜ = A˜ B, ˜ and |0˜ = |0, ˜ for all non-tilde and tilde operators (z 1 A + z 2 B)˜ = z¯ 1 A˜ + z¯ 2 B, defined on h and h˜ respectively, and z 1 , z 2 ∈ C. The zero temperature (or the limiting case of its inverse, β = ∞) phase of the system is described by the enlarged Hilbert space,

built from the Fock vacuum,

H∞ = h ⊗ h˜

(5.77)

˜ |0∞  = |0 ⊗ |0

(5.78)

by actions of the ladder operators a, a † , a, ˜ a˜ † , such that a |0∞  = a˜ |0∞  = 0 .

(5.79)

Temperature is introduced via thermal Bogoliubov transformations of the algebra generators, ˜ b˜ † }0 0. Thus, the expectation value V does not vanish when V = 0, implying the existence of a non-vanishing minimum37 Vo of V throughout the evolution. Physically, in the context of homogeneous and isotropic cosmology, this means that the singularity has been resolved, and that the effective evolution displays a bounce, with a non-zero minimum of the spatial volume. Further, this ensures a transition between two phases of the universe characterised by the sign sgn(ζ j ), describing a contracting universe (sgn(ζ j ) < 0) and an expanding one (sgn(ζ j ) > 0). Each of these phases behaves according to the general relativistic FLRW evolution in the classical and non-thermal limits (5.185), that is, when ζ j (equivalently the condensate contribution n co ( j) to the volume) becomes very large with respect to all the constants of motion and the thermal contributions. However, as expected, these two phases display a non-standard evolution in general, especially when close to the bounce. This is the regime where ζ j is comparable in magnitude to the other quantities present in the model. This leads to the particularly important question about the presence of accelerated expansion and its magnitude. To address this question, we proceed with a simplified analysis, where we make the approximation of selecting a single spin mode [33, 81], thus dropping the sum over all spins in the various expressions. In this case, the generalised equations of motion (5.177) and (5.178) reduce to, 

V

V



2 = 4M + 4

E j ζ j2 − Q 2j − 2Mζ j2 s 2j − Ms 4j

(ζ j2 + s 2j )2   E j − 2Ms 2j V

= 4M + 2 . V ζ j2 + s 2j

 (5.192) (5.193)

Now, the magnitude of a phase of accelerated expansion can be estimated in terms of: the number of e-folds38 [81] given by,

This is indeed a minimum since 0 < V

|n oco . This is analogous to the standard expression for the number of e-folds in classical general relativity,   aend Vend 1/3 N = ln = ln abeg Vbeg

37 38

where a = V 1/3 is the scale factor in terms of spatial volume.

150

5 Thermal Group Field Theory

    end 1 Vend n co + n th 1 = ln N := ln beg 3 Vbeg 3 n co + n th

(5.194)

where Vbeg and Vend are the average total volumes at the beginning and end of the phase of accelerated expansion respectively; and, in terms of an acceleration39 parameter [81] given by,   5 V 2 V

− a := . (5.195) V 3 V Using Eqs. (5.192) and (5.193) above, we get     n 2Q + n 2th 10 n co 20 1− + M . 3 n co + n th 3 (n co + n th )2 (5.196) Assuming that the bounce is the starting point of the expansion phase, we have 8 a = − M + 2M 3



n E − 2n th n co + n th

o n beg co = n co

(5.197)

for any j. Then, it is straightforward to check that acceleration is positive at the beginning, i.e. a|beg > 0, as required. Now, the end of accelerated expansion is characterised by a|end = 0 , which gives, n end co

3 7 = n th − n E + 4 8



 49 2 5 9  2 n E + n 2Q + n th − n E n th 64 2 16

(5.198)

assuming an expanding phase of the universe, i.e. Vend > Vbeg , and non-negativity of n end co even when n th is negligible. The number of e-folds can thus be estimated by,

e3N =

7 4

   49 2  2  9 n th − 21 n E + 64 n th − n E n th n E + 25 n 2Q + 16 .    n th − 21 n E + 41 n 2E + n 2Q

(5.199)

Since the quantities n E , n Q and n th are all independent, we can observe three interesting regimes, giving approximate numerical values for N : 39

This is motivated by the expression for acceleration in classical GR. We recall that in spatially flat Friedmann cosmology with a massless scalar field φ, the relative acceleration with respect to proper time τ , written in terms of φ-derivatives is given by # 2 #  2 $   $ a¨ 1  π φ  2 ∂φ V 1 V¨ 2 V˙ 5 ∂φ V 2 = = − − a 3 V 3 V 3 V V 3 V

where, dots denote τ -derivatives, V = a 3 , πφ is conjugate momentum of scalar field φ, and φ˙ = πφ /V has been used to change variables from τ to φ. We refer to [81, 95] for details.

5.3 Thermal Condensate Cosmology

n th , n Q  n E : n th , n E  n Q : n E , n Q  n th :

151

  7 1 ln ≈ 0.186 3 4   5 1 ≈ 0.152 N ≈ ln 6 2   5 1 ≈ 0.305 N ≈ ln 3 2 N ≈

(5.200) (5.201) (5.202)

The upper bound on N in the previous zero temperature free theory analysis [81] is 0.186, while here for finite β free theory it is 0.305, achieved in an early time limit. This difference is attributed to the only new aspect that we have introduced in the model, the thermal cloud of quanta of geometry. This shows that the number of e-folds can be increased, even without a non-linear dynamics. This fact is in contrast with the previous conclusions [81], that non-linear interaction terms in the GFT action are necessary to increase N . The interaction terms are naturally accompanied by their corresponding coupling constants. These are free parameters which can then be fine-tuned to essentially give the desired value for N , as in [81]. However, it remains true that the increase in N achieved in our present case is very minimal, and still not sufficient to match the physical estimates of N ∼ 60. Nevertheless, we expect this to be overcome by going beyond a static thermal cloud. In other words, a dynamical thermal cloud, which would be expected to be left over from a geometrogenesis phase transition (of an originally unbroken, pre-geometric phase), could have the potential to provide a viable mechanism for an extended phase of geometric inflation. We note that the implementation of dynamical statistical fluctuations would require special care in order to avoid pathological behaviours with regards to the use of relational clock functions t (φ). This would be in addition to the standard requirement of having a stable macroscopic phase, wherein fluctuations in the relevant observables are sufficiently subdominant or even decaying, throughout the evolution of the universe. We briefly discuss the issue of extending to a dynamical thermal cloud in Sect. 5.3.6 below, but its complete investigation is left to future work. Finally, we expect that removing the restriction to a single spin mode in the calculation above, would not alter the qualitative conclusion that a static thermal cloud is insufficient to generate a satisfactory number of e-folds to match the observational estimate. However, a relaxation of the condition (5.186) for sgn(ζ j ), by considering a non-homogeneous distribution of the sign with respect to the modes j while preserving the classical limit manifest in the emergence of Friedmann equations at large volumes, might give rise to a larger ratio between the volumes at the end and at the beginning of the phase of accelerated expansion, and consequently a larger number of e-folds.

152

5 Thermal Group Field Theory

5.3.6 Remarks We have presented above an effective, relational homogeneous and isotropic cosmological model based on the use of a condensate phase with fluctuating geometric volume, and an introduction of reference clock functions. In particular, we have considered a non-interacting class of group field theory models, and condensates that are characterised by non-dynamical thermal clouds. Below, we conclude with some discussions surrounding these two aspects, namely having an overall free dynamics and considering a thermal condensate with a static cloud, which are in fact mutually related. There are three main features of our specific choice of state, namely a coherent thermal state of the form (5.125) at inverse temperature β. Firstly, β is assumed to be constant. Secondly, the average number of quanta in this state splits neatly into a condensate and a non-condensate part, such that the zero temperature limit gives a pure β-independent condensate (see also Eq. (5.135)), i.e. a † aβ = n co + n non-co lim a aβ = n co †

β→∞

(5.203) (5.204)

where in the present work the non-condensate part is taken to be thermal and at equilibrium at inverse temperature β. Having such a split is not only convenient in doing computations but also adds clarity to the expressions in subsequent analyses when considering the interplays between the two. Moreover, having this β → ∞ limit is crucial for recovering the results of past studies in GFT cosmology. Thirdly, the expectation value of the field operator in a coherent thermal state is temperature independent, i.e.   (5.205) aχ α σ,σ¯ ;β = σχα  = aχ α σ thus being identical to the zero temperature case. At first sight this seems contrary to our expectation that the condensate would be affected by the presence of a thermal cloud, which is indeed true in general. But what is also true is that, the independence of σχα  from β in the present case, is entirely compatible with our current approximation of neglecting interactions and taking β constant. We know that when temperature is switched on, quanta from the condensate are depleted into the thermal cloud. Now in a generally interacting case, both the thermal cloud and the condensate are interacting and dynamical by themselves, while also interacting with each other. However, in the case of free dynamics, the thermal cloud will not interact with the condensate part, in addition to the quanta also being free within each part separately. Thus even though our state includes a thermal cloud, the coherent condensate part (described fully by its order parameter σ ) will be unaffected by it, indeed as depicted by Eq. (5.205) above. This is further reasonable in light of having a constant β, because if temperature were to change, say to increase, then we would expect more quanta to be depleted into the

5.3 Thermal Condensate Cosmology

153

thermal cloud, and thus expect the state of the condensate, i.e. its order parameter, to also change. So overall, considering this class of states, in which the order parameter is temperature independent, is a reasonable approximation when the temperature is constant and interactions are neglected. Not including interactions ensures that the thermal cloud doesn’t affect the condensate, while constant β ensures that the amount of depletion is also constant, so together the condensate can indeed be approximated by a β-independent order parameter. In such a case we may be missing out on some interesting physics, however we take this case as a first step towards further investigations in the future. Finally, we note that the interesting case of a dynamically changing β is also left for future studies. In such a case, the expected dominance of the condensate part over the thermal cloud at late times would not only be determined by a dynamically increasing condensate (as is the case in the present work), but also by what would be a dynamically decreasing temperature as the universe expands.

Appendix 1: Gibbs States for Positive Extensive Generators We show that the operator e−β(P−μN ) (see Eq. (5.3)) is bounded, positive and traceclass on H F , and subsequently calculate its trace. Notice that it is self-adjoint by definition, due to the self-adjointness of the exponent. In the following, we use the  orthonormal occupation number basis {{n χi αi } } as introduced in Sect. 4.1.2, and denote the modes by i ≡ χi , α i for convenience [9]. Lemma 1. Operator e−β(P−μN ) is bounded in the operator norm on H F , for 0 < β < ∞ and μ ≤ λ0 , where λ0 = min(λχ,  α ) and P as defined in (5.1). Proof 1. An operator A is called bounded if there exists a real k ≥ 0 such that ||Aψ|| ≤ k||ψ|| for all ψ in the relevant Hilbert space. Recall that, e−β(P−μN ) |{n i } = e−β



i (λi −μ)n i

|{n i }

(5.206)

  where, {n χi αi } are the basis vectors. Then, for a generic state |ψ =

 {n i }

with coefficients ci ∈ C, we have

c{ni } |{n i } ∈ H F

(5.207)

154

5 Thermal Group Field Theory

||e−β(P−μN ) ψ||2 = ||



c{ni } e−β



i (λi −μ)n i

{n i }

=



|{n i } ||2



c¯{ni } c{ni } e−β

i (λi −μ)n i

e−β

(5.208) 

i (λi −μ)n i

{n i }|{n i }

{n i },{n i }

=



2 −2β

|c{ni } | e



i (λi −μ)n i

≤

{n i }



(5.209) |c{ni } | = ||ψ|| 2

2

(5.210)

{n i } 

using orthonormality of basis; and, 0 < e−2β 0, where μ ≤ λi for all i).

i (λi −μ)n i

≤ 1 (since β



i (λi

− μ)n i ≥ 

Lemma 2. Operator e−β(P−μN ) is positive on H F , for 0 < β < ∞ and μ ≤ λ0 . Proof 2. A bounded self-adjoint operator A is positive if ψ|Aψ ≥ 0 for all ψ in the relevant Hilbert space. Then, for any ψ ∈ H F , we have 

ψ| e−β(P−μN ) |ψ =

c¯{ni } c{ni } {n i }| e−β

{n i },{n i }

=



|c{ni } |2 e−β



i (λi −μ)n i



i (λi −μ)n i

≥ 0.

|{n i }

(5.211) (5.212)

{n i }

 Lemma 3. Operator e−β(P−μN ) is trace-class on H F , for 0 < β < ∞ and μ < λ0 . Further, its trace is given by, Z β,μ =

 χ,  α

1 1−

e−β(λχ α −μ)

(5.213)

as in Eq. (5.4). Proof 3.40 A bounded operator A on a Hilbert space is trace-class if Tr(|A|) < ∞, √ where |A| := A† A. Further, for a self-adjoint positive A, we have41 Tr(A) < ∞ ⇒ Tr(|A|) < ∞ .

(5.214)

40

This proof is along the lines of that reported in [9], but is detailed here further, for grand-canonicaltype states, for clarity and consistency. 41 We remark that there is, in fact, an iff equivalence between the following: for any bounded operator B, and some orthonormal basis {en } in a complex Hilbert space, we have [30, 96]  ||Ben || < ∞ ⇔ Tr(|B|) < ∞ . n

However for the purposes of the present proof, we only need the forward implication and the result (5.217), i.e. the implication shown in (5.214).

5.3 Thermal Condensate Cosmology

155

One way to see the validity of (5.214) is as follows [30, 64, 96, 97]. Let {ei } be an orthonormal basis in a complex Hilbert space, such that A |ei  = ai |ei . Notice that, for self-adjoint positive A, we have 

||Aei || =



i

(ei , A† Aei ) =

i



(ei , A2 ei )

(5.215)

i

=

 ai2

(5.216)

i

=



ai = Tr(A)

(5.217)

i

where we have used the self-adjointness of A in (5.215), and positivity in (5.217). Then,   Tr(|A|) = (ei , |A|ei ) ≤ |(ei , |A|ei )| (5.218) i

i

≤



|| |A|ei ||

(5.219)

||Aei || = Tr(A)

(5.220)

i

=

 i

where we have used the Cauchy-Schwarz inequality in (5.219), result (5.217) in (5.220), and the following identity [97], || |A|ψ ||2 = (ψ, |A|2 ψ) = (ψ, A† Aψ) = ||Aψ||2

(5.221)

for any vector ψ in the given Hilbert space. Thus Tr(|A|) ≤ Tr(A), which implies (5.214). In our case with A = e−β(P−μN ) , it is therefore sufficient to show that Tr(e−β(P−μN ) ) converges in H F . Then, Tr(e−β(P−μN ) ) =

 

{n i }| e−β(P−μN ) |{n i }

(5.222)

e−β{ni } N

(5.223)

N ≥0 {n i }| N

=

 

N ≥0 {n i }| N

where we have denoted, {ni } N ≡

 (λi − μ)n i .

(5.224)

i

The  second sum in (5.222) is restricted to those microstates |{n i } with a fixed N = αi . This can be understood as summing over all possible ways of arranging i n χi , N particles into an arbitrary number of boxes, each labelled by a single mode i =

156

5 Thermal Group Field Theory

(χi , α i ). Notice that the dominant contribution to this sum comes from the state with the minimum . This is the ground state |N , 0, 0, . . ., in which all N particles occupy the single-particle ground state of P (for a fixed μ) with eigenvalue λ0 . Then, 0 = (λ0 − μ)N

(5.225)

characterises the N -particle ground state. Let us separate this contribution to rewrite the sum as,   e−β{ni } N = e−β0 + e−β{ni } N (5.226) {n i }| N

|{n i } =|N ,0,...

where now all sub-dominant terms are e−β{ni } N < e−β0 . Further, we can rearrange the states in the sum (on the right hand side in (5.226)) according to increasing values of , and denote these with tildes in the new sequence, to get 

e−β{ni } N

=



%

e−β {ni }l,N

%{n } >0  i l,N

|{n i } =|N ,0,...



≡

%

e−β l,N .

(5.227)

%l,N >0 

Index l ∈ {1, 2, 3, . . .} labels the reorganised list of N -particle states in ascend%l+1,N , where equality refers to possi%l,N ≤  ing order of their eigenvalues, i.e.  ble degeneracies in adjacent states in the sequence. This can be taken into account explicitly by a further rewriting, as 

%

e−β l,N =

%l,N >0 



%

g L e−β L ,N

(5.228)

% L ,N >0 

% L , and we have where now, L ∈ {1, 2, 3, . . .} labels the level set with eigenvalue  % L ,N <  % L+1,N ,  % L ,N <  % L ,N +1 . 

(5.229)

g L is the degree of degeneracy42 of the level L, which is assumed to be finite for ˜ every L, and such that it increases less than exponentially with increasing . Together, we have the double series Tr(e−β(P−μN ) ) =

 

%

g L e−β L ,N

(5.230)

% L ,N ≥0 N ≥0 

% L=0 = 0 . where now, we have allowed for degeneracy in 0 (for generality), and  Each (so-called row and column) series, of the above double series, converges by ratio test, 42

Degree of degeneracy is the dimension of the eigenspace of the degenerate states, or equivalently, the multiplicity of the corresponding spectral value.

5.3 Thermal Condensate Cosmology

lim

L→∞

157

g L+1 −β( % L+1,N − % L ,N ) e < 1, gL

%

%

lim e−β(L ,N +1 −L ,N ) < 1 .

N →∞

Therefore, the double series in (5.230) converges absolutely [98].

(5.231) 

We remark that the above proof can be applied directly to the analogous case of canonical states of the form (5.2), to show that they are trace-class in a given N particle Hilbert space [9]. The trace can be evaluated straightforwardly, exactly along the lines of calculation of a grand-canonical partition function for an ideal Bose gas in standard quantum statistical mechanics. In occupation number basis, we have Tr(e−β(P−μN ) ) =



e−β



i (λi −μ)n i

(5.232)

{n i }

=



e−β(λ0 −μ)n 0 e−β(λ1 −μ)n 1 . . .

(5.233)

{n i }

=

∞ 

e

−β(λ0 −μ)n 0

n 0 =0

=

∞   χ,  α n χ α =0

∞ 

e−β(λ1 −μ)n 1 . . .

(5.234)

n 1 =0

e−β(λχ α −μ)n χ α =

 χ,  α

1 . 1 − e−β(λχ α −μ)

(5.235) 

Remark. The above Proofs 1–3 are directly applicable to the analogous case of self-adjoint extensive operators P with discrete spectrum that are semi-bounded on H F , instead of simply being positive. Being semi-bounded essentially means that the spectrum is either bounded from below or from above. In the case when P is bounded from below, i.e. ∃ a minimum eigenvalue λ0 (be it non-negative or negative), then the corresponding grand-canonical state satisfies the above proofs for 0 < β < ∞ and μ < λ0 . An example of this case is precisely the one that is considered in the above Lemmas. On the other hand, in the case when P is bounded from above, i.e. ∃ a maximum eigenvalue λ0 (be it non-negative or negative), then the corresponding grand-canonical state satisfies the above proofs for −∞ < β < 0 and μ > λ0 . An example of this case is the state (5.36) considered in Sect. 5.1.2.1, for the regularised momentum operators generating internal translations along Rn .

Appendix 2: KMS Condition and Gibbs States We consider the question of when Gibbs density operators are the unique normal KMS states. The statements of the lemma, and of the following corollary, are only slight variations of the traditional one encountered in standard algebraic quantum statistical mechanics (see Remark 1 below). The proof is directly in line with the

158

5 Thermal Group Field Theory

standard ones; specifically, we have made combined use of strategies suggested in [24, 25]. Lemma. Let A be a C*-algebra which is irreducible on a Hilbert space HA , i.e. the commutant A := {A ∈ B(HA ) | [A, B] = 0, ∀B ∈ A} is a multiple of identity, A = CI ≡ {cI | c ∈ C}. Let αt be a 1-parameter group of *-automorphisms of A which are implemented on HA by a group of unitary operators U (t) = eiGt , where t ∈ R and G is a self-adjoint operator on HA . Consider a normal algebraic state ωρ on A, i.e. ωρ [A] = Tr(ρ A) (for all A ∈ A), where ρ is a density operator on HA . Then, ωρ is an α-KMS state at value β, if and only if the corresponding density operator is of the Gibbs form, (5.236) ρ = c e−βG where, c ∈ C\{0} and β ∈ R>0 . Proof. Since ωρ is a KMS state, by definition (see page 24) we have a complex function FAB (z), for every A, B ∈ A, which satisfies the following boundary conditions, FAB (t) = Tr(ρ A eiGt Be−iGt ) FAB (t + iβ) = Tr(ρ e

iGt

Be

−iGt

A)

(5.237) (5.238)

where t = Re(z). Further by definition, FAB is analytic on I = {z ∈ C | 0 < Im(z) < ¯ for a given 0 < β < ∞. β}, and continuous and bounded on its closure I, Consider A = I . We can do this because the above conditions must hold for every pair of elements in A, thus also for this simple case. Then, we have an equality FI B (t) = FI B (t + iβ)

(5.239)

for all t ∈ R and B ∈ A. Since FI B is analytic on I, we can continuously move to another point, say z = (t + a) + ib ∈ I, where the equality will still hold, i.e. FI B (z) = FI B (z + iβ). By analytic continuation, we see that FI B is analytic on full C, and periodic along the imaginary axis, with period β. Further recall that, FI B is bounded. Therefore, FI B is bounded and analytic on C, and by Liouville’s theorem, it is constant. That is, (5.240) Tr(ρ eiGt Be−iGt ) = constant . Since this is true for all t and B, we have that the state itself is invariant, i.e. eiGt ρe−iGt = ρ

(5.241)

as expected. In this simple setting, we have basically recovered the known result that any algebraic KMS state, say ωKMS , is stationary with respect to its defining automorphism group, i.e. ωKMS [α A] = ωKMS [A] (for all A). Result (5.241) will be used in the following.

5.3 Thermal Condensate Cosmology

159

Now for any A, B ∈ A, let us consider the boundary conditions (5.238) and (5.237) as follows. For (5.238), we have FAB (t + iβ) = Tr(eiGt e−iGt ρ eiGt Be−iGt A) = Tr(e

iGt

ρ Be

= Tr(ρ B e

−iGt

−iGt

Ae

(5.242)

A)

(5.243)

)

(5.244)

iGt

using (5.241), and cyclicity of trace. For (5.237), by continuity we get FAB (t) → FAB (t + iβ) = Tr(ρ A eiG(t+iβ) Be−iG(t+iβ) ) −βG

−iGt

(5.245)

βG

)

(5.246)

= Tr(e−βG B eβG e−iGt ρ A eiGt )

(5.247)

= Tr(ρ A e = Tr(e

iGt

−βG

e

Be

βG

Be

ρe

−iGt

e

Ae

iGt

)

(5.248)

again using (5.241), and cyclicity of trace. Then from (5.248) and (5.244), we have Tr(e−βG B eβG ρ e−iGt AeiGt ) = Tr(ρ B e−iGt AeiGt )

(5.249)

which, we recall, holds for every A ∈ A, t ∈ R, by definition of a KMS state. Therefore, e−βG B eβG ρ = ρ B

⇒ B eβG ρ = eβG ρ B ⇒ [e

βG

ρ, B] = 0 (∀B ∈ A)

(5.250) (5.251)

⇒ e

βG

ρ∈A

(5.252)

⇒ e

βG

ρ = cI

(5.253)

where the last step is due to irreducibility of A on HA . Validity of the converse statement, that a Gibbs state satisfies the KMS condition, can be found detailed in numerous standard texts (see, for example [24–26], or the original papers [63, 99, 100]).  Remark 1. In standard quantum statistical mechanics for material systems on spacetime, a commonly encountered example of the above is the case of finite systems, e.g. a box of gas [24–26]. In this case, A = B(H) is the algebra of all bounded linear operators on some Hilbert space, which is naturally irreducible. Then, given the unitary group of time translations U (t) = ei H t , we have that canonical Gibbs states e−β H are the unique normal KMS states, according to the above proof. This can be extended directly for grand-canonical states, by considering instead a generator H˜ = H − μN [24, 26]. Remark 2. There are two main features of the system that are vital for this proof: existence of a 1-parameter group of unitary operators U (t) which is strongly continuous (thus, associated with a self-adjoint generator G, by Stone’s theorem); and,

160

5 Thermal Group Field Theory

irreducibility of the algebra A on a given Hilbert space. As long as any algebraic system has these two features, the above proof will follow through. Therefore, we have the following: Corollary. Let A be a C*-algebra, and π be an irreducible representation of A, with GNS Hilbert space Hπ . By irreducibility we have, π(A) = CI . Let αt be a 1-parameter group of automorphisms of A, which are implemented by a strongly continuous group of unitary operators U (t) = eiGt on Hπ . Then, the unique normal KMS state, with respect to U (t) at value β, on the algebra π(A) is a Gibbs state, of the form e−βG .

Appendix 3: Strong Continuity of Map U X Lemma. Let G be a Lie group with Lie algebra G, H be a Hilbert space, and U(H) be the group of unitary operators on H, as considered in Sect. 5.1.2.1. Given a continuous map g X : R → G, t → g X (t), and a strongly continuous map U : G → U(H), g → U (g), then U X := U ◦ g X : t → U X (t) is strongly continuous in H, i.e. ||(U X (t1 ) − U X (t2 ))ψ|| → 0 as t1 → t2

(5.254)

for a given X ∈ G, any t1 , t2 ∈ R, and all ψ ∈ H. [9] Proof. Recall that, by strong continuity of U we have ||(U (g1 ) − U (g2 ))ψ|| → 0 as g1 → g2

(5.255)

for any g1 , g2 ∈ G and all ψ ∈ H. Then, for any t1 , t2 ∈ R and all ψ ∈ H, we have ||(U X (t1 ) − U X (t2 ))ψ|| = ||(U (g X (t1 )) − U (g X (t2 )))ψ|| = ||(U (g1 ) − U (g2 ))ψ||

(5.256) (5.257)

where g1 ≡ g X (t1 ) and g1 ≡ g X (t2 ) are arbitrary elements on the curve g X (t) ∈ G. Now, by continuity of g X , we have g1 → g2 as t1 → t2 . Then, using strong continuity of U in (5.255), we have ||(U (g1 ) − U (g2 ))ψ|| → 0 , as t1 → t2 .

(5.258) 

5.3 Thermal Condensate Cosmology

161

Appendix 4: Normalisation of Gibbs State for Closure Condition Lemma. The partition function for the generalised Gibbs state ρβ (Eq. (5.51)) on {A I } with respect to the closure condition, is given by Zβ =

4  4π A I

||β||

I =1

sinh(A I ||β||)

(5.259)

as in Eq. (5.53). Proof. This proof follows the strategy presented in [44], for the analogous case of action of 3d rotations on a single sphere. Recall that, β ∈ su(2), {A I } = S 2A1 × · · · ×  S 2A4  m, and A I ∈ R>0 ; J (m) := 4I =1 X I ∈ su(2)∗ is a smooth dual algebravalued function on {A I } , with ||X I || = A I ; and, β.J (m) is a smooth real-valued function on {A I } . Then, the partition function is Zβ =

dλ e−β·J

{A I }

= =

S 2A 1



...

4  I =1

S 2A 4

[dμ]4 e−

(5.260) 4

I =1

β.X I

dμ e−β.X I S 2A

(5.261)

(5.262)

I

where dμ is an area element on a single 2-sphere with a fixed radius A I . We can naturally embed this system in Euclidean R3 , by identifying both su(2) and su(2)∗ with R3 ,43 and taking the surface measure on a single sphere as that induced  x , is the by R3 . Then, for any b ∈ su(2), x ∈ su(2)∗ , the inner product, b.x = b. usual dot product for 3d vectors. Now, let β ≡ β be an arbitrary non-zero vector in su(2) ∼ = R3 . Further, let us choose an orthonormal cartesian frame (ex , ey , ez ) in R3 , such that β = ||β||ez (5.263) where ||β|| ∈ R>0 . Recall that by definition, a point m = (X I ) ∈ {A I } identifies four points (or equivalently, the associated vectors) X I ∈ S 2A I , one each on the individual 2-spheres. Any such vector X I can be written in spherical coordinates (θ, φ), for 43

There exists a canonical isomorphism between 3d vectors and rotation matrices (i.e. adjoint rep3 resentation of su(2) or so(3)) given by: R3  b = (b1 , b2 , b3 ) → bˆ = a=1 ba Lˆ a ∈ su(2), where ˆL a are matrix generators of 3d rotations. Equivalently, in the standard cartesian basis, the isomorphism is: ex , ey , ez → Lˆ 1 , Lˆ 2 , Lˆ 3 . The Lie bracket structure on R3 is given by the standard cross product: [bˆ , bˆ ] = b ∧ b . 1

2

1

2

162

5 Thermal Group Field Theory

fixed radius A I , as X I = A I (sin θ cos φ ex + sin θ sin φ ey + cos θ ez )

(5.264)

where, θ ∈ [0, π ], φ ∈ [0, 2π ] as per common convention. The standard area element in this parametrization is (5.265) dμ = A2I sin θ dθ dφ . Then, the contribution to Z β from each integral with fixed I is given by,

 

S 2A

dμ e−β. X = A2





2π

π

dφ 0

dθ sin θ e−A||β|| cos θ

(5.266)

0

2π A2 A||β|| = du eu A||β|| −A||β||   4π A e A||β|| − e−A||β|| = ||β|| 2 4π A sinh(A||β||) = ||β||

where, we have substituted u := −A||β|| cos θ .

(5.267) (5.268) (5.269) 

References 1. Kuhn TS (1987) Black-body theory and the quantum discontinuity, 1894-1912. University of Chicago Press 2. Oriti D (2016) Group field theory as the 2nd quantization of Loop Quantum Gravity. Class Quant Grav 33(8):085005. https://doi.org/10.1088/0264-9381/33/8/085005 3. Pithis AGA, Sakellariadou M (2019) Group field theory condensate cosmology: an appetizer. Universe 5(6). ISSN 2218-1997. https://doi.org/10.3390/universe5060147. https:// www.mdpi.com/2218-1997/5/6/147 4. Oriti D (2017) The universe as a quantum gravity condensate. Comptes Rendus Physique 18:235–245. https://doi.org/10.1016/j.crhy.2017.02.003 5. Gielen S, Sindoni L (2016) Quantum cosmology from group field theory condensates: a review. SIGMA 12:082. https://doi.org/10.3842/SIGMA.2016.082 6. Gabbanelli L, De Bianchi S (2021) Cosmological implications of the hydrodynamical phase of group field theory. Gen Relativ Gravit 53(7):66. https://doi.org/10.1007/s10714-02102833-z 7. Fetter AL, Walecka JD (1971) Quantum theory of many-particle systems. International series in pure and applied physics. McGraw-Hill. https://books.google.de/books? id=Y1HwAAAAMAAJ 8. Ashtekar A, Lewandowski J (1998) Quantum theory of geometry. 2. Volume operators. Adv Theor Math Phys 1:388–429 9. Kotecha I, Oriti D (2018) Statistical equilibrium in quantum gravity: Gibbs states in group field theory. New J Phys 20(7):073009. https://doi.org/10.1088/1367-2630/aacbbd 10. Assanioussi M, Kotecha I (2020) Thermal quantum gravity condensates in group field theory cosmology. Phys Rev D 102(4):044024. https://doi.org/10.1103/PhysRevD.102.044024

References

163

11. Bianchi E, Dona P, Speziale S (2011) Polyhedra in loop quantum gravity. Phys Rev D 83:044035. https://doi.org/10.1103/PhysRevD.83.044035 12. Haggard HM (2011) Asymptotic analysis of spin networks with applications to quantum gravity. PhD thesis, UC, Berkeley. http://escholarship.org/uc/item/93t675vk 13. Carlo R, Lee S (1995) Discreteness of area and volume in quantum gravity. Nucl Phys B 442:593–622. https://doi.org/10.1016/0550-3213(95)00550-5. [Erratum: Nucl Phys B456:753 (1995)]. https://doi.org/10.1016/0550-3213(95)00150-Q 14. Assanioussi M, Kotecha I (2020) Thermal representations in group field theory: squeezed vacua and quantum gravity condensates. JHEP 20:173. https://doi.org/10.1007/ JHEP02(2020)173 15. Montesinos M, Rovelli C (2001) Statistical mechanics of generally covariant quantum theories: a Boltzmann-like approach. Class Quant Grav 18:555–569. https://doi.org/10.1088/ 0264-9381/18/3/314 16. Krasnov KV (1997) Geometrical entropy from loop quantum gravity. Phys Rev D 55:3505– 3513. https://doi.org/10.1103/PhysRevD.55.3505 17. Astuti V, Christodoulou M, Rovelli C (2019) Volume entropy. Class Quant Grav 36(5):055012. https://doi.org/10.1088/1361-6382/aafec7 18. Perez A (2017) Black holes in loop quantum gravity. Rept Prog Phys 80(12):126901. https:// doi.org/10.1088/1361-6633/aa7e14 19. Diaz-Polo J, Pranzetti D (2012) Isolated horizons and black hole entropy in loop quantum gravity. SIGMA 8:048. https://doi.org/10.3842/SIGMA.2012.048 20. Pitaevskii L, Stringari S (2003) Bose-Einstein condensation. Oxford University Press, Oxford 21. Wilson-Ewing E (2019) A relational Hamiltonian for group field theory. Phys Rev D 99(8):086017. https://doi.org/10.1103/PhysRevD.99.086017 22. Gielen S (2016) Emergence of a low spin phase in group field theory condensates. Class Quant Grav 33(22):224002. https://doi.org/10.1088/0264-9381/33/22/224002 23. Pithis AGA, Sakellariadou M, Tomov P (2016) Impact of nonlinear effective interactions on group field theory quantum gravity condensates. Phys Rev D 94(6):064056. https://doi.org/ 10.1103/PhysRevD.94.064056 24. Haag R (1992) Local quantum physics: fields, particles, algebras. Springer, texts and monographs in physics, Berlin, Germany 25. Emch GG (1980) An algebraic approach for spontaneous symmetry breaking in quantum statistical mechanics. In: Kramer P, Cin MD (eds) Groups, systems and many-body physics. Vieweg+Teubner Verlag, Wiesbaden, pp 246–284. ISBN 978-3-663-06825-9. https://doi.org/ 10.1007/978-3-663-06825-9_5 26. Strocchi F (2008) Symmetry breaking. Lect Notes Phys, 732:1–216. https://doi.org/10.1007/ 978-3-540-73593-9 27. Rovelli C (1993) Statistical mechanics of gravity and the thermodynamical origin of time. Class Quant Grav 10:1549–1566. https://doi.org/10.1088/0264-9381/10/8/015 28. Connes A, Rovelli C (1994) Von Neumann algebra automorphisms and time thermodynamics relation in general covariant quantum theories. Class Quant Grav 11:2899–2918. https://doi. org/10.1088/0264-9381/11/12/007 29. Fecko M (2006) Differential geometry and lie groups for physicists. Cambridge University Press, Cambridge. https://doi.org/10.1017/CBO9780511755590 30. Moretti V (2017) Spectral theory and quantum mechanics: mathematical foundations of quantum theories, symmetries and introduction to the algebraic formulation; 2nd edn. Unitext. Springer, Cham. https://doi.org/10.1007/978-3-319-70706-8 31. Bisognano JJ, Wichmann EH (1976) On the duality condition for quantum fields. J Math Phys 17:303–321. https://doi.org/10.1063/1.522898 32. Li Y, Oriti D, Zhang M (2017) Group field theory for quantum gravity minimally coupled to a scalar field. Class Quant Grav 34(19):195001. https://doi.org/10.1088/1361-6382/aa85d2 33. Oriti D, Sindoni L, Wilson-Ewing E (2016) Emergent Friedmann dynamics with a quantum bounce from quantum gravity condensates. Class Quant Grav 33(22):224001. https://doi.org/ 10.1088/0264-9381/33/22/224001

164

5 Thermal Group Field Theory

34. Woit P (2017) Quantum theory, groups and representations. Springer. ISBN 978-3-319-646107, 978-3-319-64612-1. https://doi.org/10.1007/978-3-319-64612-1 35. Gieres F (2000) Mathematical surprises and Dirac’s formalism in quantum mechanics. Rep Prog Phys 63(12):1893–1931. https://doi.org/10.1088/0034-4885/63/12/201 36. Dimock J (2011) Quantum mechanics and quantum field theory: a mathematical primer. Cambridge University Press, Cambridge. https://doi.org/10.1017/CBO9780511793349 37. Chirco G, Kotecha I, Oriti D (2019) Statistical equilibrium of tetrahedra from maximum entropy principle. Phys Rev D 99(8):086011. https://doi.org/10.1103/PhysRevD.99.086011 38. Chirco G, Kotecha I (2019) Generalized Gibbs ensembles in discrete quantum gravity. In: Nielsen F, Barbaresco F (eds) Geometric science of information 2019. Lecture Notes in Computer Science (LNCS). Springer, Cham 39. Kapovich M, Millson JJ (1996) The symplectic geometry of polygons in euclidean space. J Differ Geom 44(3):479–513. https://doi.org/10.4310/jdg/1214459218 40. Barbieri A (1998) Quantum tetrahedra and simplicial spin networks. Nucl Phys B 518:714– 728. https://doi.org/10.1016/S0550-3213(98)00093-5 41. Baez JC, Barrett JW (1999) The quantum tetrahedron in three-dimensions and fourdimensions. Adv Theor Math Phys 3:815–850. https://doi.org/10.4310/ATMP.1999.v3.n4. a3 42. Conrady F, Freidel L (2009) Quantum geometry from phase space reduction. J Math Phys 50:123510. https://doi.org/10.1063/1.3257109 43. Souriau J-M (1997) Structure of dynamical systems: a symplectic view of physics, vol 149. Springer Science & Business Media. https://doi.org/10.1007/978-1-4612-0281-3. Translation of Structure des Systemes Dynamiques (1969). Dunod 44. Marle C-M (2016) From tools in symplectic and poisson geometry to J.-M. Souriau’s theories of statistical mechanics and thermodynamics. Entropy 18(10). ISSN 1099-4300. https://doi. org/10.3390/e18100370. http://www.mdpi.com/1099-4300/18/10/370 45. Chirco G, Laudato M, Mele FM (2021) Covariant momentum map thermodynamics for parametrized field theories. Int J Geom Meth Mod Phys 18(02):2150018. https://doi.org/ 10.1142/S0219887821500183 46. Chirco G, Laudato M, Mele FM (2019) Multi-symplectic lie group thermodynamics for covariant field theories. In: Nielsen F, Barbaresco F (eds) Geometric science of information. Springer, Cham. ISBN 978-3-030-26980-7 47. Kotecha I (2019) Thermal quantum spacetime. Universe 5(8):187. https://doi.org/10.3390/ universe5080187 48. Freidel L, Speziale S (2010) Twisted geometries: a geometric parametrisation of SU(2) phase space. Phys Rev D 82:084040. https://doi.org/10.1103/PhysRevD.82.084040 49. Rovelli C, Speziale S (2010) On the geometry of loop quantum gravity on a graph. Phys Rev D 82:044018. https://doi.org/10.1103/PhysRevD.82.044018 50. Regge T, Williams RM (2000) Discrete structures in gravity. J Math Phys 41:3964–3984. https://doi.org/10.1063/1.533333 51. Regge T (1961) General relativity without coordinates. Nuovo Cim 19:558–571. https://doi. org/10.1007/BF02733251 52. Dittrich B, Speziale S (2008) Area-angle variables for general relativity. New J Phys 10:083006. https://doi.org/10.1088/1367-2630/10/8/083006 53. Perez A (2012) The new spin foam models and quantum gravity. Papers Phys 4:040004. https://doi.org/10.4279/PIP.040004 54. Baratin A, Oriti D (2012) Group field theory and simplicial gravity path integrals: a model for Holst-Plebanski gravity. Phys Rev D 85:044003. https://doi.org/10.1103/PhysRevD.85. 044003 55. Finocchiaro M, Oriti D (2020) Spin foam models and the Duflo map. Class Quant Grav 37(1):015010. https://doi.org/10.1088/1361-6382/ab58da 56. Baratin A, Oriti D (2010) Group field theory with non-commutative metric variables. Phys Rev Lett 105:221302. https://doi.org/10.1103/PhysRevLett.105.221302

References

165

57. Baratin A, Dittrich B, Oriti D, Tambornino J (2011) Non-commutative flux representation for loop quantum gravity. Class Quant Grav 28:175011. https://doi.org/10.1088/0264-9381/28/ 17/175011 58. Takahasi Y, Umezawa H (1975) Thermo field dynamics. Collect Phenom 2:55–80. Reprint https://doi.org/10.1142/S0217979296000817 59. Matsumoto H (1985) Thermo field dynamics and its development. In: Ezawa H, Kamefuchi S (eds) Progress in quantum field theory. Elsevier Science Publishers B. V 60. Umezawa H, Matsumoto H, Tachiki M (1982) Thermo field dynamics and condensed states. North-holland, Amsterdam, Netherlands 61. Umezawa H (1993) Advanced field theory: micro, macro, and thermal physics. AIP, New York, USA 62. Khanna FC, Malbouisson APC, Malbouisson JMC, Santana AR (2009) Thermal quantum field theory - algebraic aspects and applications. World Scientific, New Jersey. http://ebooks. worldscinet.com/ISBN/9789812818898/9789812818898.html 63. Haag R, Hugenholtz NM, Winnink M (1967) On the equilibrium states in quantum statistical mechanics. Commun Math Phys 5:215–236. https://doi.org/10.1007/BF01646342 64. Bratteli O, Robinson DW (1987) Operator algebras and quantum statistical mechanics. Vol 1: C* and W* algebras, symmetry groups, decomposition of states, 2nd edn. Springer, Berlin Heidelberg 65. Bratteli O, Robinson DW (1997) Operator algebras and quantum statistical mechanics. Vol 2: equilibrium states, models in quantum statistical mechanics, 2nd edn. Springer, Berlin Heidelberg 66. Ojima I (1981) Gauge fields at finite temperatures: thermo field dynamics, KMS condition and their extension to gauge theories. Ann Phys 137:1. https://doi.org/10.1016/00034916(81)90058-0 67. Landsman NP, van Weert CG (1987) Real and imaginary time field theory at finite temperature and density. Phys Rept 145:141. https://doi.org/10.1016/0370-1573(87)90121-9 68. Celeghini E, De Martino S, De Siena S, Iorio A, Rasetti M, Vitiello G (1998) Thermo field dynamics and quantum algebras. Phys Lett A244:455–461. https://doi.org/10.1016/S03759601(98)00447-2 69. Nielsen MA, Chuang IL (2010) Quantum computation and quantum information. Cambridge University Press, Cambridge. https://doi.org/10.1017/CBO9780511976667 70. Raamsdonk MV (2017) Lectures on gravity and entanglement. In: Proceedings, theoretical advanced study institute in elementary particle physics: new frontiers in fields and strings (TASI 2015): Boulder, CO, USA, June 1-26, 2015, pp 297–351. https://doi.org/10.1142/ 9789813149441_0005 71. Chapman S, Eisert J, Hackl L, Heller MP, Jefferson R, Marrochio H, Myers RC (2019) Complexity and entanglement for thermofield double states. SciPost Phys 6(3):034. https:// doi.org/10.21468/SciPostPhys.6.3.034 72. Maldacena JM (2003) Eternal black holes in anti-de Sitter. JHEP 04:021. https://doi.org/10. 1088/1126-6708/2003/04/021 73. Israel W (1976) Thermo field dynamics of black holes. Phys Lett A 57:107–110. https://doi. org/10.1016/0375-9601(76)90178-X 74. Kay BS (1985) The double wedge algebra for quantum fields on Schwarzschild and Minkowski space-times. Commun Math Phys 100:57. https://doi.org/10.1007/BF01212687 75. Sewell GL (1982) Quantum fields on manifolds: PCT and gravitationally induced thermal states. Ann Phys 141:201–224. https://doi.org/10.1016/0003-4916(82)90285-8 76. Kegeles A, Oriti D, Tomlin C (2018) Inequivalent coherent state representations in group field theory. Class Quant Grav 35(12):125011. https://doi.org/10.1088/1361-6382/aac39f 77. Barnett SM, Knight PL (1985) Thermofield analysis of squeezing and statistical mixtures in quantum optics. J Opt Soc Am B Opt Phys 2:467–479. https://doi.org/10.1364/JOSAB.2. 000467 78. Mann A, Revzen M (1989) Thermal coherent states. Phys Lett A 134(5):273–275. ISSN 0375-9601. https://doi.org/10.1016/0375-9601(89)90635-X. http://www.sciencedirect.com/ science/article/pii/037596018990635X

166

5 Thermal Group Field Theory

79. Oz-Vogt J, Mann A, Revzen M (1991) Thermal coherent states and thermal squeezed states. J Mod Opt 38(12):2339–2347. https://doi.org/10.1080/09500349114552501 80. Gielen S, Oriti D (2018) Cosmological perturbations from full quantum gravity. Phys Rev D 98(10):106019. https://doi.org/10.1103/PhysRevD.98.106019 81. de Cesare M, Pithis AGA, Sakellariadou M (2016) Cosmological implications of interacting group field theory models: cyclic universe and accelerated expansion. Phys Rev D94(6):064051. https://doi.org/10.1103/PhysRevD.94.064051 82. Gielen S (2019) Inhomogeneous universe from group field theory condensate. JCAP 02:013. https://doi.org/10.1088/1475-7516/2019/02/013 83. Engel E, Dreizler RM (2013) Density functional theory: an advanced course. Theoretical and mathematical physics. Springer, Berlin Heidelberg 84. Parr RG, Yang W (1994) Density-functional theory of atoms and molecules. Oxford University Press, USA 85. Marchetti L, Oriti D (2021) Effective relational cosmological dynamics from quantum gravity. JHEP 05:025. https://doi.org/10.1007/JHEP05(2021)025 86. Höhn PA, Smith ARH, Lock MPE (2019) The trinity of relational quantum dynamics. https:// doi.org/10.1103/PhysRevD.104.066001 87. Höhn PA, Vanrietvelde A (2020) How to switch between relational quantum clocks. New J Phys 22(12):123048. https://doi.org/10.1088/1367-2630/abd1ac 88. Höhn PA (2019) Switching internal times and a new perspective on the ‘wave function of the universe’. Universe 5(5):116. https://doi.org/10.3390/universe5050116 89. Gielen S, Polaczek A (2021) Hamiltonian group field theory with multiple scalar matter fields. Phys Rev D 103(8):086011. https://doi.org/10.1103/PhysRevD.103.086011 90. Adjei E, Gielen S, Wieland W (2018) Cosmological evolution as squeezing: a toy model for group field cosmology. Class Quant Grav 35(10):105016. https://doi.org/10.1088/13616382/aaba11 91. Gielen S (2014) Quantum cosmology of (loop) quantum gravity condensates: an example. Class Quant Grav 31:155009. https://doi.org/10.1088/0264-9381/31/15/155009 92. Gielen S, Oriti D, Sindoni L (2013) Cosmology from group field theory formalism for quantum gravity. Phys Rev Lett 111(3):031301. https://doi.org/10.1103/PhysRevLett.111.031301 93. Gielen S, Oriti D, Sindoni L (2014) Homogeneous cosmologies as group field theory condensates. JHEP 06:013. https://doi.org/10.1007/JHEP06(2014)013 94. Oriti D, Sindoni L, Wilson-Ewing E (2017) Bouncing cosmologies from quantum gravity condensates. Class Quant Grav 34(4):04LT01. https://doi.org/10.1088/1361-6382/aa549a 95. de Cesare M, Sakellariadou M (2017) Accelerated expansion of the Universe without an inflation and resolution of the initial singularity from group field theory condensates. Phys Lett B 764:49–53. https://doi.org/10.1016/j.physletb.2016.10.051 96. Beltrametti EG, Cassinelli G, Carruthers PA (1984) The logic of quantum mechanics, vol 15. Encyclopedia of mathematics and its applications. Cambridge University Press, Cambridge. https://doi.org/10.1017/CBO9781107340725 97. Reed M, Simon B (1981) Functional analysis, vol 1. Methods of Modern Mathematical Physics, Elsevier Science. ISBN 9780080570488 98. Ghorpade SR, Limaye BV (2010) A course in multivariable calculus and analysis. Springer Science & Business Media. https://doi.org/10.1007/978-1-4419-1621-1 99. Kubo R (1957) Statistical mechanical theory of irreversible processes. 1. General theory and simple applications in magnetic and conduction problems. J Phys Soc Jap 12:570–586. https:// doi.org/10.1143/JPSJ.12.570 100. Martin PC, Schwinger JS (1959) Theory of many particle systems. 1. Phys Rev 115:1342– 1373. https://doi.org/10.1103/PhysRev.115.1342

Chapter 6

Conclusions

Knowledge is love and light and vision. —Helen Keller

In this thesis, we have discussed: aspects of a generalised framework for equilibrium statistical mechanics in the context of background independent systems; and, thermal aspects of a candidate quantum spacetime composed of many combinatorial and algebraic quanta, utilising their field theoretic formulation of group field theory. Specifically, we have focussed on generalisation of Gibbs states [1–6].

6.1 Towards Generalised Equilibrium Statistical Mechanics We have presented aspects of a potential extension of equilibrium statistical mechanics for background independent systems with an arbitrarily large but finite number of degrees of freedom. In particular, we have focused on the definition of equilibrium states, based on a collection of results and insights from studies of constrained systems on spacetime and discrete quantum gravitational systems devoid of standard spacetime-related structures. While various proposals for a generalised notion of statistical equilibrium have been summarised (Sects. 2.2.1 and 2.2.2), one in particular, based on the constrained maximisation of information entropy has been stressed upon (Sect. 2.2.3). As we have detailed, this characterisation is in the spirit of Jaynes’ method, wherein the constraints are average values of a set of macroscopic observables {Oa  = Ua } that an observer has access to, and maximising the entropy under these constraints amounts to finding the least-biased distribution over the microscopic states such that the statistical averages of the same Oa coincide with

© The Author(s), under exclusive license to Springer Nature Switzerland AG 2022 I. Kotecha, On Generalised Statistical Equilibrium and Discrete Quantum Gravity, Springer Theses, https://doi.org/10.1007/978-3-030-90969-7_6

167

168

6 Conclusions

their given macroscopic values Ua . The resultant state is a generalised Gibbs density function or operator (Eqs. (2.31) and (2.34) respectively), characterised by a set of several observables and a conjugate multivariable temperature. Further, we have discussed how this notion of equilibrium in a generalised Gibbs state, and its associated stationarity with respect to the modular flow, is democratic, in that it does not require preferring any one of these observables as special over the others (Sect. 2.2.4). We have also investigated preliminary aspects of a generalised thermodynamics as directly implied by these states, including defining the basic thermodynamic potentials (Sect. 2.3.1), considering the issue of deriving a single common temperature (Sect. 2.3.2), and discussing generalised zeroth and first laws (Sect. 2.3.3). We have argued in favour of the potential of this thermodynamical characterisation based on the maximum entropy principle, by highlighting its many unique and valuable features (Sect. 2.2.5). For instance, this characterisation is comprehensive, accommodating all past proposals for defining Gibbs states. It is also inherently observer-dependent, being defined using the observed macrostate {Oa  = Ua }. Further, this method does not require a pre-defined automorphism to define equilibrium with respect to, unlike the KMS characterisation. Although, once a state has been defined, one can (if one wants) extract its modular flow with respect to which it will satisfy the KMS condition (Sect. 2.2.4). Therefore, this proposal could be especially useful in quantum gravitational contexts (Chap. 5), where we may be interested in geometric quantities such as area and volume (Sect. 5.1.1) which may not necessarily be generators of some automorphism of a system a priori. An important extension of our considerations, for future work, is a suitable inclusion of constrained dynamics and its consequences, before any deparametrization. For example, the considerations in Sect. 5.1.3, associated with classical constraint functions, require a more complete understanding as to their interpretation in terms of effective constraints and their applications [7–10]. Aspects of generalised thermodynamics also require further development. For instance in the first law as presented in Sect. 2.3.3, the additional possible work contributions need to be identified and understood, particularly in the context of background independence, along with the interpretation of generalised heat terms [11–14]. It would also be interesting to understand better the roles of and relation to (quantum) information, entropy and (macroscopic) observers in these contexts [15–23], and the relation to quantum reference frames [24–30]. Such investigations into generalised statistical and thermodynamical aspects may benefit from working with some specific, physically motivated example, for example stationary black holes. For instance, the thermodynamical characterisation could be applied in a spacetime setting, with respect to the mass, charge and angular momentum observables, like we alluded to in the Introduction. In addition to clarifying some of the aspects that we mentioned above, such a setting could further help unfold the physical mechanism for the selection of a single common temperature, thus also of physical time and energy, starting from a generalised Gibbs measure where none is preferred a priori. This may also have an illuminating interplay with quantum reference frames in spacetime [28, 31–33].

6.2 Towards Thermal Quantum Spacetime

169

6.2 Towards Thermal Quantum Spacetime 6.2.1 Many-Body Formulation and Group Field Theory We have considered equilibrium statistical mechanical aspects of a candidate quantum gravitational system, composed of many quanta of geometry. The choice of these quanta is inspired directly from boundary structures in various discrete approaches including loop quantum gravity, spin foams and simplicial gravity. They are the combinatorial building blocks (i.e. boundary patches) of graphs, labelled with algebraic data (usually of group SU (2)) encoding discrete geometric information (Sects. 3.1 and 4.1), e.g. labelled 4-valent nodes or tetrahedra in 4d models. Their many-body dynamics is dictated by non-local interaction vertices (Sects. 3.2 and 3.4), e.g. 4simplices in 4d models, resulting in a discrete quantum spacetime, e.g. 4d simplicial complex. Statistical states can then be defined on a multi-particle state space e.g. of an arbitrarily large but finite number of tetrahedra. Then, generalised Gibbs states can be defined using the thermodynamical characterisation in general, or if a suitable 1-parameter group of automorphism exists then equivalently using the dynamical KMS condition characterisation (Sects. 3.3 and 5.1). In particular, we have shown that a coarse-graining (using coherent states) of a class of generalised Gibbs states of a system of such quanta of geometry, with respect to the dynamics-encoding kinetic and vertex operators, naturally gives rise to covariant group field theories (Sect. 3.4). In this way, we have interpreted a group field theory as an effective statistical field theory, extracted from the underlying statistical quantum gravitational system, and have thus provided a statistical basis for the standard understanding of these quanta as being excitations of group fields. In this thesis, we have considered complex-valued scalar group fields, defined over a domain space comprised of locally compact, connected and unimodular Lie groups. In particular, we have considered domain manifolds of the general form G d × Rn , with integers d ≥ 1 and n ≥ 0 (Sects. 3.1 and 4.1). In some specific examples, we have chosen G = SU (2), d = 4 and n = 1, corresponding to some common choices for 4-dim GFT models, minimally coupled to a single real-valued scalar matter field (Sect. 4.1). The dynamics of group fields is encoded in an action function (or from a statistical standpoint, an effective Hamiltonian or a Landau-Ginzburg free energy function), with a non-local interaction term defining the bulk vertex of the 2-complex (equivalently, of the GFT Feynman diagram), and a local kinetic term defining the propagator associated with bulk bondings between these vertices (Sect. 3.2). The many-body perspective has been our main technical strategy for the development and investigation of thermal equilibrium aspects of group field theory, in a fully background independent context for the fundamental candidate building blocks of quantum spacetime, and within the full theory as opposed to special approximations. Specifically, this perspective has offered advantages at two levels. First, the suggested formal description of spacetime as a many-body quantum system has allowed us to handle these issues within a mathematical formalism that maintains close analogies with that used for more standard physical systems. This, in a way, has permitted us

170

6 Conclusions

to move forward without having fully solved all the conceptual issues, especially surrounding background independence, implicated in the problem. Second, while GFTs are background independent from the point of view of spacetime physics (in the sense that spacetime itself has to be reconstructed in most of its features), their mathematical definition as field theories on Lie groups has allowed us to work with the background structures of the group manifold playing technically a very similar role to what spacetime structures play in usual field theories, e.g. for condensed matter systems. Along this line, we have first established the ground work for the system’s classical and quantum kinematics, to later consider its statistical aspects. Specifically, we have described a Weyl algebraic formulation for the choice of bosonic quanta (Sect. 4.1.3), presented the required details of the Fock representation associated with a degenerate vacuum (Sects. 4.1.1 and 4.1.2), and constructed groups of unitarily implementable translation *-automorphisms (Sect. 4.1.4) to be used later for defining structural equilibrium states. We have also outlined a procedure to deparametrize an originally constrained many-body system, to define from it a canonical Hamiltonian system equipped with a good clock variable (Sect. 4.2).

6.2.2 Generalised Gibbs States Based on the above many-body framework, we have constructed examples of statistical Gibbs states for discrete quantum geometries composed of classical and quantum tetrahedra, and in general polyhedra (Sect. 5.1). As a first example of applying the thermodynamical characterisation, we have presented a class of Gibbs density operators generated by extensive, positive (more generally, semi-bounded either from above or below, see the Remark in Appendix 1 in Chap. 5) operators defined on the Fock Hilbert space of the degenerate vacuum (Sect. 5.1.1.1). As a special case, we have discussed a state associated with a geometric volume operator (Sect. 5.1.1.2). Such a state can be understood as describing a quantum gravitational state underlying a region of space with fixed macroscopic (average) volume. We have shown that a direct consequence of a system being in such a state, is the occurrence of Bose-Einstein condensation to the single-particle ground state of the volume operator, much like the case of non-relativistic Bose gases characterised by a free Hamiltonian. We have thus presented a model-independent, statistical mechanism for generating a low spin phase (e.g. spin-1/2, when neglecting the degenerate spin-0 case, for SU (2) data), starting from a thermal state. Such phases are encountered often in studies related to group field theory and loop quantum gravity. For further work along this line, it would be interesting to study quantum black hole states of these degrees of freedom, with thermality potentially associated with area operators [34–38]. In general, as we have stressed before, it is important to be able to identify suitable observables to characterise an equilibrium state of physically relevant cases with. Further investigating thermodynamics of quantum gravitational

6.2 Towards Thermal Quantum Spacetime

171

systems would benefit from confrontation with studies of thermodynamics of spacetime [39–42]. For this we may need to consider the quantum nature of the degrees of freedom, and use insights from the field of quantum thermodynamics [43], which itself has interesting links to quantum information theory [44]. Then, we have considered the KMS condition characterisation for generalised Gibbs states. Along the lines of arguments in standard algebraic quantum statistical mechanics, we have clarified that the unique normal KMS states in an algebraic system (which is not necessarily GFT) are Gibbs states, when the algebra of observables is irreducible on the given Hilbert space and the system is equipped with a strongly continuous 1-parameter group of unitary transformations (Appendix 2 in Chap. 5). Subsequently, we have identified the same structures in the present GFT system, for the construction of (unique KMS) Gibbs states. Specifically, we have constructed two classes of Gibbs states associated with momentum operators (Sect. 5.1.2), which satisfy the KMS condition with respect to 1-parameter groups of transformations defined previously in Sects. 4.1.4 and 4.2. In the first (Sect. 5.1.2.1), we have considered 1-parameter groups of translations on the base manifold G d × Rn , and have constructed structural Gibbs states associated with their corresponding self-adjoint momentum operators. These states encode equilibrium with respect to internal translations along the base manifold. Since the group manifold is in general curved, then naturally the corresponding notion of thermality depends on the trajectory used to define it, just like in the case of Rindler trajectories on Minkowski spacetime. For the second class of states (Sect. 5.1.2.2), we recall that the primary reason to couple scalar fields, by extending the base manifold of group fields by R degrees of freedom, was to subsequently use them to define relational clock reference frames. It was then natural to seek Gibbs states, still generated by the momentum of the scalar field, but within a deparametrized system thus encoding relational dynamics. With this in mind, we have presented relational physical Gibbs states defined with respect to clock Hamiltonians, based on the result of deparametrization as detailed earlier in Sect. 4.2. Lastly, we have considered classical equilibrium configurations of a system of many tetrahedra, using the thermodynamical characterisation for constraint functions. The main idea here is that the imposition of constraints can be understood from a statistical standpoint, either being satisfied strongly (i.e. exactly, C = 0) via a microcanonical distribution on the extended unconstrained phase space, or effectively (i.e. on average, C = 0) via a canonical Gibbs state (Sect. 5.1.3). We have considered two examples for preliminary investigations. However, further work is required to understand physical consequences of our examples in quantum gravity; and to understand better the implementation and consequences of effective constraints, C, in quantum gravity [7–10]. As a first example, we have considered the simple case of the classical closure condition associated with a single tetrahedron (Sect. 5.1.3.1). The corresponding Gibbs distribution then describes a tetrahedron geometry fluctuating in terms of its closure; and is characterised by a vector-valued temperature β ∈ su(2). It is an example of Souriau’s definition of Gibbs states for Lie group actions [11, 12], here associated with the closure constraint generating a diagonal SU (2) action. We have

172

6 Conclusions

left further investigation of the application of this state in simplicial gravity to future work. Another interesting extension would be to explore aspects of its Lie group thermodynamics, in line with the studies stemming from Souriau’s generalisation of Gibbs states [11–14]. As another example with motivations rooted more directly in simplicial gravity, we have considered formal Gibbs distributions in a system of many tetrahedra, with respect to area-matching gluing constraints between adjacent triangular faces. This has produced fluctuating twisted geometric configurations for connected simplicial complexes formed by the same tetrahedra (Sect. 5.1.3.2). This line of investigation can be used to explore specific examples of simplicial gravity (or group field theory) models with direct or stronger geometric interpretation, and thus of greater interest for quantum gravity. For instance, one could consider the state space of geometric (in the sense of metric) tetrahedra and utilise a generalised Gibbs state to define the partition function with a dynamics encoded by the Regge action [45, 46]. Another interesting direction would be to define a Gibbs density implementing not only gluing constraints but also shape-matching constraints [47], or simplicity constraints, on the twisted geometry space [48, 49], thus reducing to a proper Regge geometry starting from SU (2) holonomy-flux data.

6.2.3 Thermofield Double Vacua and Inequivalent Representations In Sect. 5.2, we have constructed finite temperature, equilibrium phases associated with a class of generalised Gibbs states in group field theory, based on their nonperturbative thermal vacua. For this, we have utilised tools from the formalism of thermofield dynamics (Sect. 5.2.1). The vacua are squeezed states encoding entanglement of quantum geometric data (Sect. 5.2.3), and are unitarily inequivalent to the class of degenerate vacua (Sect. 5.2.2). Entanglement is expected to be a characteristic property of a physical quantum description of spacetime in general [15, 50–63]. This setup also opens the door to using such techniques in discrete quantum gravity, thus facilitating exploration of the phase structure of quantum gravity models characterised by generalised thermodynamic parameters βa ; and, complementing renormalization investigations in group field theory [64–66] and possibly other related approaches [67–69]. Further, we have introduced coherent thermal states which, in addition to carrying statistical fluctuations in a given set of observables, are also condensates of quantum geometry (Sect. 5.2.4). Zero temperature coherent states in group field theory have been used to obtain an effective description of flat, homogeneous and isotropic cosmology (flat FLRW), where certain quantum corrections arise naturally and generate a dynamical modification with respect to classical gravity, preventing the occurrence of a big bang singularity along with cyclic solutions in general [70–73]. Encouraged by these results, the introduction of statistical condensates, like coherent thermal

6.2 Towards Thermal Quantum Spacetime

173

states, may bring further progress to the GFT condensate cosmology program by offering a tangible and controllable way of incorporating perturbations in relevant observables. Such considerations could be valuable say for understanding the quantum gravitational origin of structure formation. They could also lead to modifications during early times in the previously studied homogeneous and isotropic flat cosmology models in GFT, such as altering the inflation rate [6, 70, 74], as considered later in Sect. 5.3. The thermal vacua constructed here (Sect. 5.2.3) are thermofield double states [42, 75–80]. This setup could thus also be useful for the study of quantum black holes. In group field theory for example, black holes have been modelled as generalised condensates [35, 36], which must also possess related thermal properties. Thermal coherent states may then provide just the right type of technical structure, in order to study the statistical and thermal aspects of the corresponding quantum black holes [35–38]. It would also be interesting to understand better the connection of these vacua with similar works in loop quantum gravity concerning kinematical entanglement between intertwiners in spin networks, and related further to discrete vector geometries [57, 58, 81], especially since the squeezed vacua constructed here essentially encode entanglement between gauge-invariant spin network nodes (i.e. intertwiners), but at a field theory level. Moreover, our construction can be extended even further to more general two-mode squeezed vacua. For instance, condensates of correlated quanta, like dipole condensates [72], may be straightforwardly constructed and studied in this setup. Considering correlations between different modes of the quanta, which encode quantum geometric data, might also make comparisons with the studies in LQG mentioned above [57, 58, 81] more direct. Finally, by providing quite a straightforward handle on collective, quasi-particle modes in discrete quantum gravity, while still allowing for access to different inequivalent representations, this framework may bring closer the studies of microscopic theories of quantum gravity and analogue gravity models [82].

6.2.4 Condensate Cosmology with Volume Fluctuations As a preliminary application in a more physically relevant setting, we have studied some implications of the presence of statistical volume fluctuations in the context of group field theory by using coherent thermal states for condensate cosmology (Sect. 5.3). In the GFT condensate cosmology program, a quantum gravitational phase of the universe is modelled as a condensate. Along these lines, we have considered a thermal condensate (Sect. 5.3.1), consisting of: a pure condensate representing an effective macroscopic homogeneous spacetime, like in previous studies [70–73]; and, a static thermal cloud over the pure condensate part, encoding statistical fluctuations of quantum geometry. The presented model recovers cosmological dynamics of a flat FLRW universe with a minimally coupled scalar field at late times (Sect. 5.3.5.2), when the con-

174

6 Conclusions

densate dominates the thermal cloud. While at early times (Sect. 5.3.5.3), when the thermal part dominates the condensate, the model displays quantum and statistical corrections, the latter being the primary difference with respect to earlier works based on pure (zero temperature, or non-thermal) condensates. In particular, we have shown that the singularity is generically resolved with a bounce between a contracting and an expanding phase, and that there exists an early phase of accelerated expansion (Sect. 5.3.5.3). The expansion phase is characterised by an increased number of efolds compared to those achieved in the previous zero temperature analysis of the same class of free GFT models. This increase in the number of e-folds, obtained in absence of interactions, is attributed to the presence of the thermal cloud. This is in contrast to previous conclusions (see [74] and related works) that an increase in the number of e-folds necessarily requires non-zero interactions. However, the maximum number of e-folds achieved here (≈ 0.3) are still negligible. Thus, considering a dynamical thermal cloud and non-trivial interactions would be expected to result in a sufficiently long period of this geometric inflation. These would be valuable extensions of the present work. Consideration of a dynamical (non-static) thermal cloud would allow for further investigations of consequences of the presence of a thermal cloud on the effective physics of the system, even in free models. Subsequently, it would naturally be interesting to consider an interacting model in the presence of thermal fluctuations. In fact, these aspects of having a dynamical thermal cloud and an overall interacting theory are intimately related, as discussed briefly in Sect. 5.3.6. In general, one could systematically extend the previous studies in GFT condensate cosmology [71– 73] to the case with thermal fluctuations using our setup, and investigate various aspects including dynamical analysis of fluctuations, perturbations, anistropies and inhomogeneities. For our analysis, we have introduced a suitable generalisation of relational clock frames in GFT, by considering clock functions t (φ), implemented as smearing functions (Sect. 5.3.3). Consequently, we have formulated the effective equations of motion and the dynamical quantities as functionals of t (Sect. 5.3.4). In comparison with past works where relational quantities are functions of the coordinate φ, the clock frames introduced here resolve divergences associated with coincidence limits φ1 → φ2 . A more complete understanding of relational frames in GFT and their precise occurrence from a physical mechanism of deparametrization is left to future work. Lastly, we have understood β as a statistical parameter that controls the extent of depletion of the condensate into the thermal cloud, and overall the strength of statistical fluctuations of observables in the system. The question remains whether it also admits a geometrical interpretation. Taking guidance from classical general relativity, we know that spatial volume generates a dynamical evolution in constant mean curvature foliations, wherein the temporal evolution is given by the so-called York time parameter. Constant York time slices are thus constant extrinsic curvature scalar (mean curvature) slices, and the two quantities are proportional to each other. In this case, one could attempt to understand β as the periodicity in York time, equivalently in scalar extrinsic curvature (both of which are conjugates to the spa-

6.2 Towards Thermal Quantum Spacetime

175

tial volume). In particular for homogeneous and isotropic spacetimes, York time is further proportional to the Hubble parameter [83]. A detailed investigation of such aspects and their implications would be interesting for future work, also for studying thermodynamical aspects of the present quantum gravitational system.

6.3 Final Remarks We have asked the question: can we characterise a macroscopic system as being in equilibrium without there being a notion of time? And we have tentatively answered: yes; if the system has maximum total entropy, compatible with its macrostate (e.g. average volume, energy, etc.), then we can say that it is in equilibrium. In traditional statistical thermodynamics, this is a direct consequence of the second law. Thus, the validity of the second law ensures the validity of this characterisation for statistical equilibrium. But in this thesis, in the context of background independent systems, we have understood this “thermodynamical characterisation” as being more fundamental, coinciding with the understanding of the quality of entropy in a macroscopic dynamical system as being more fundamental than an evolution parameter (i.e. time), the latter being a feature only of the special class of deparametrized (or deparametrizable) constrained systems. We are accustomed to understanding (and subsequently treating) statistical equilibrium as being synonymous with the property of stationarity in time,1 often to the extent that the property of maximal entropy is understood as simply being an additional feature of an equilibrium configuration that is not fundamental to its definition. However in the context of dynamically constrained (or time reparametrization-invariant) systems, wherein a preferred, external, global choice of a time variable is absent, the latter property of maximal entropy may be more definitive. The justification of this suggestion must naturally lie in its consequences for physical systems, both gravitational and non-gravitational. Since we have arrived at this suggestion in our attempts to define Gibbs states (and therefore, also understand their construction procedures) within the context of the present discrete quantum gravitational system, our investigations are also limited accordingly. In particular, much like in almost any approach to quantum gravity, our investigations largely face a disconnect from established spacetime physics (even though we have made preliminary attempts at connecting with a candidate macroscopic phase and cosmology, in Sects. 5.2 and 5.3). This disconnect is especially stark in more radical approaches that are not based on standard spacetime structures, and is tied with the difficult open problem of emergence of spacetime; in this thesis, we have not directly tackled the problem of emergence, however our results may provide some useful tools

1

Or, with the property of satisfying Kubo’s correlation functions, i.e. the KMS boundary conditions, with respect to the given time evolution.

176

6 Conclusions

to address it.2 Therefore, the following two broad but important directions call for further work: physical consequences of generalised statistical equilibrium in quantum gravity and connection with known spacetime phenomena; and, investigation of generalised statistical equilibrium in constrained systems on spacetime3 . Moreover, these tasks of formulating a framework for background independent statistical mechanics, applicable also to gravity (since like any other dynamical field, gravitational field must also undergo thermal fluctuations), and that of investigating the statistical mechanics of quanta of geometry are formally different. We have dealt with the latter.4 The conceptual challenges, like timelessness, that are encountered when considering the statistical mechanics of general relativistic spacetime, and of pre-geometric quanta underlying a spacetime (as defined in some quantum gravity framework) are similar. But they are two separate issues, even if expected to be related eventually5 ; and, developments in one can lead to a more refined understanding of the other. Finally, we recognise that insights from statistical mechanics and thermodynamics were crucial for the birth of the quantum hypothesis by Planck,6 and thus of quantum theory. They may prove to be crucial also in our quest for understanding the fundamental nature of gravity.

References 1. Kotecha I, Oriti D (2018) Statistical equilibrium in quantum gravity: gibbs states in group field theory. New J Phys 20(7):073009. https://doi.org/10.1088/1367-2630/aacbbd 2. Chirco G, Kotecha I, Oriti D (2019) Statistical equilibrium of tetrahedra from maximum entropy principle. Phys Rev D 99(8):086011. https://doi.org/10.1103/PhysRevD.99.086011 3. Chirco G, Kotecha I (2019) Generalized gibbs ensembles in discrete quantum gravity. In: Nielsen F, Barbaresco F (eds) Geometric science of information 2019. Lecture notes in computer science (LNCS). Springer, Cham 4. Kotecha I (2019) Thermal quantum spacetime. Universe 5(8):187. https://doi.org/10.3390/ universe5080187 5. Assanioussi M, Kotecha I (2020) Thermal representations in group field theory: squeezed vacua and quantum gravity condensates. JHEP 20:173. https://doi.org/10.1007/JHEP02(2020)173 6. Assanioussi M, Kotecha I (2020) Thermal quantum gravity condensates in group field theory cosmology. Phys Rev D 102(4):044024. https://doi.org/10.1103/PhysRevD.102.044024 7. Bojowald M, Sandhofer B, Skirzewski A, Tsobanjan A (2009) Effective constraints for quantum systems. Rev Math Phys 21:111–154. https://doi.org/10.1142/S0129055X09003591 2

A quantum statistical framework can indeed be used, starting from a given quantum gravitational model, to extract and analyse the collective behaviour of the underlying degrees of freedom. It is at this coarse-grained level of description that we expect continuum spacetime and geometry to emerge [84–86]. 3 We note that this latter case has been studied in some works, e.g. [11–14, 87]. 4 For efforts toward the former, see for example [13, 14, 87–93]. 5 Even then, to uncover this explicit relation, and see the interplay with spacetime physics, would require tackling the issue of emergence more directly. 6 For interesting discussions, see for instance [94, 95].

References

177

8. Bojowald M, Tsobanjan A (2009) Effective constraints for relativistic quantum systems. Phys Rev D 80:125008. https://doi.org/10.1103/PhysRevD.80.125008 9. Bojowald M, Hoehn PA, Tsobanjan A (2011) An Effective approach to the problem of time. Class Quant Grav 28:035006. https://doi.org/10.1088/0264-9381/28/3/035006 10. Bojowald M, Hoehn PA, Tsobanjan A (2011) Effective approach to the problem of time: general features and examples. Phys Rev D 83:125023. https://doi.org/10.1103/PhysRevD.83.125023 11. Souriau J-M (1997) Structure of dynamical systems: a symplectic view of physics, vol 149. Springer Science & Business Media. . https://doi.org/10.1007/978-1-4612-0281-3. Translation of Structure des Systemes Dynamiques, 1969. Dunod 12. Marle C-M (2016) From tools in symplectic and poisson geometry to J.-M. Souriau’s theories of statistical mechanics and thermodynamics. Entropy 18(10). ISSN 1099-4300. https://doi. org/10.3390/e18100370. http://www.mdpi.com/1099-4300/18/10/370 13. Chirco G, Laudato M, Mele FM (2021) Covariant momentum map thermodynamics for parametrized field theories. Int J Geom Meth Mod Phys 18(02):2150018. https://doi.org/10. 1142/S0219887821500183 14. Chirco G, Laudato M, Mele FM (2019) Multi-symplectic lie group thermodynamics for covariant field theories. In: Nielsen F, Barbaresco F (eds) Geometric science of information. Springer, Cham. ISBN 978-3-030-26980-7 15. Hoehn PA (2017) Reflections on the information paradigm in quantum and gravitational physics. J Phys Conf Ser 880(1):012014. https://doi.org/10.1088/1742-6596/880/1/012014 16. Zeilinger A (1999) A foundational principle for quantum mechanics. Found Phys 29(4):631– 643. https://doi.org/10.1023/A:1018820410908 ˇ Zeilinger A (2003) Information and fundamental elements of the structure of 17. Brukner C, quantum theory. In: Castell L, Ischebeck O (eds) Time, quantum and information. Springer, Berlin Heidelberg, pp 323–354. ISBN 978-3-662-10557-3. https://doi.org/10.1007/978-3662-10557-3_21 18. Jaynes ET (1992) The Gibbs paradox. In: Ray Smith C, Erickson GJ, Neudorfer PO (eds) Maximum entropy and bayesian methods. Springer, Netherlands, Dordrecht, pp 1–21. ISBN 978-94-017-2219-3. https://doi.org/10.1007/978-94-017-2219-3_1 19. Fuchs CA (2002) Quantum mechanics as quantum information (and only a little more). arXiv:quant-ph/0205039 20. Rovelli C (2017) Is time’s arrow perspectival? In: Saunders S, Silk J, Barrow JD, Chamcham K (eds) The philosophy of cosmology. Cambridge University Press, pp 285–296. https://doi. org/10.1017/9781316535783.015 ˇ (2014) Quantum causality. Nat Phys 10(4):259–263. https://doi.org/10.1038/ 21. Brukner C nphys2930 22. Spekkens RW (2007) Evidence for the epistemic view of quantum states: a toy theory. Phys Rev A 75:032110. https://doi.org/10.1103/PhysRevA.75.032110 23. Spekkens RW (2016) Quasi-quantization: classical statistical theories with an epistemic restriction. In: Chiribella G, Spekkens RW (eds) Quantum theory: informational foundations and foils. Springer, Netherlands, Dordrecht, pp 83–135. ISBN 978-94-017-7303-4. https://doi.org/ 10.1007/978-94-017-7303-4_4 ˇ (2019) Quantum mechanics and the covariance of 24. Giacomini F, Castro-Ruiz E, Brukner C physical laws in quantum reference frames. Nat. Commun. 10(1):494. https://doi.org/10.1038/ s41467-018-08155-0 25. Vanrietvelde A, Hoehn PA, Giacomini F, Castro-Ruiz E (2020) A change of perspective: switching quantum reference frames via a perspective-neutral framework. Quantum 4:225. ISSN 2521-327X. https://doi.org/10.22331/q-2020-01-27-225 26. de la Hamette A-C, Galley TD (2020) Quantum reference frames for general symmetry groups. Quantum 4:367. https://doi.org/10.22331/q-2020-11-30-367 27. Krumm M, Hoehn PA, Mueller MP (2020) Quantum reference frame transformations as symmetries and the paradox of the third particle. arXiv:2011.01951 28. Höhn PA, Smith ARH, Lock MPE (2019) The trinity of relational quantum dynamics. https:// doi.org/10.1103/PhysRevD.104.066001

178

6 Conclusions

29. Hoehn PA, Lock MPE, Ahmad SA, Smith ARH, Galley TD (2021) Quantum relativity of subsystems. arXiv:2103.01232 30. Bartlett SD, Rudolph T, Spekkens RW (2007) Reference frames, superselection rules, and quantum information. Rev Mod Phys 79:555–609. https://doi.org/10.1103/RevModPhys.79. 555 31. Giacomini F (2021) Spacetime quantum reference frames and superpositions of proper times. Quantum 5:508. https://doi.org/10.22331/q-2021-07-22-508 32. Smith ARH, Ahmadi M (2020) Quantum clocks observe classical and quantum time dilation. Nature Commun. 11(1):5360. https://doi.org/10.1038/s41467-020-18264-4 ˇ (2020) Quantum clocks and the tem33. Castro-Ruiz E, Giacomini F, Belenchia A, Brukner C poral localisability of events in the presence of gravitating quantum systems. Nat. Commun. 11(1):2672. https://doi.org/10.1038/s41467-020-16013-1 34. Krasnov KV (1997) Geometrical entropy from loop quantum gravity. Phys Rev D 55:3505– 3513. https://doi.org/10.1103/PhysRevD.55.3505 35. Oriti D, Pranzetti D, Sindoni L (2018) Black holes as quantum gravity condensates. Phys Rev D 97(6):066017. https://doi.org/10.1103/PhysRevD.97.066017 36. Oriti D, Pranzetti D, Sindoni L (2016) Horizon entropy from quantum gravity condensates. Phys Rev Lett 116:211301. https://doi.org/10.1103/PhysRevLett.116.211301 37. Diaz-Polo J, Pranzetti D (2012) Isolated horizons and black hole entropy in loop quantum gravity. SIGMA 8:048. https://doi.org/10.3842/SIGMA.2012.048 38. Perez A (2017) Black holes in loop quantum gravity. Rept Prog Phys 80(12):126901. https:// doi.org/10.1088/1361-6633/aa7e14 39. Jacobson T (1995) Thermodynamics of space-time: the Einstein equation of state. Phys Rev Lett 75:1260–1263. https://doi.org/10.1103/PhysRevLett.75.1260 40. Bardeen JM, Carter B, Hawking SW (1973) The Four laws of black hole mechanics. Commun Math Phys 31:161–170. https://doi.org/10.1007/BF01645742 41. Padmanabhan T (2010) Thermodynamical aspects of gravity: new insights. Rept Prog Phys 73:046901. https://doi.org/10.1088/0034-4885/73/4/046901 42. Israel W (1976) Thermo field dynamics of black holes. Phys Lett A 57:107–110. https://doi. org/10.1016/0375-9601(76)90178-X 43. Vinjanampathy S, Anders J (2016) Quantum thermodynamics. Contemp Phys 57(4):545–579. https://doi.org/10.1080/00107514.2016.1201896 44. Goold J, Huber M, Riera A, del Rio L, Skrzypczyk P (2016) The role of quantum information in thermodynamics—a topical review. J Phys A Math Theor 49(14):143001. https://doi.org/ 10.1088/1751-8113/49/14/143001 45. Regge T, Williams RM (2000) Discrete structures in gravity. J Math Phys 41:3964–3984. https://doi.org/10.1063/1.533333 46. Regge T (1961) General relativity without coordinates. Nuovo Cim 19:558–571. https://doi. org/10.1007/BF02733251 47. Dittrich B, Speziale S (2008) Area-angle variables for general relativity. New J Phys 10:083006. https://doi.org/10.1088/1367-2630/10/8/083006 48. Freidel L, Speziale S (2010) Twisted geometries: a geometric parametrisation of SU(2) phase space. Phys Rev D 82:084040. https://doi.org/10.1103/PhysRevD.82.084040 49. Rovelli C, Speziale S (2010) On the geometry of loop quantum gravity on a graph. Phys Rev D 82:044018. https://doi.org/10.1103/PhysRevD.82.044018 50. Bombelli L, Koul RK, Lee J, Sorkin RD (1986) A quantum source of entropy for black holes. Phys Rev D 34:373–383. https://doi.org/10.1103/PhysRevD.34.373 51. Srednicki M (1993) Entropy and area. Phys Rev Lett 71:666–669. https://doi.org/10.1103/ PhysRevLett.71.666 52. Ryu S, Takayanagi T (2006) Holographic derivation of entanglement entropy from AdS/CFT. Phys Rev Lett 96:181602. https://doi.org/10.1103/PhysRevLett.96.181602 53. Raamsdonk MV (2010) Building up spacetime with quantum entanglement. Gen Rel Grav 42:2323–2329. https://doi.org/10.1142/S0218271810018529. [Int J Mod Phys D19:2429 (2010)]. https://doi.org/10.1007/s10714-010-1034-0

References

179

54. Raamsdonk MV (2017) Lectures on gravity and entanglement. In: Proceedings, theoretical advanced study institute in elementary particle physics: new frontiers in fields and strings (TASI 2015): Boulder, CO, USA, June 1-26, 2015, pp 297–351. https://doi.org/10.1142/ 9789813149441_0005 55. Marolf D (2017) The Black Hole information problem: past, present, and future. Rept Prog Phys 80(9):092001. https://doi.org/10.1088/1361-6633/aa77cc 56. Bianchi E, Myers RC (2014) On the architecture of spacetime geometry. Class Quant Grav 31:214002. https://doi.org/10.1088/0264-9381/31/21/214002 57. Baytas B, Bianchi E, Yokomizo N (2018) Gluing polyhedra with entanglement in loop quantum gravity. Phys Rev D 98(2):026001. https://doi.org/10.1103/PhysRevD.98.026001 58. Livine ER (2018) Intertwiner entanglement on spin networks. Phys Rev D 97(2):026009. https://doi.org/10.1103/PhysRevD.97.026009 59. Chirco G, Mele FM, Oriti D, Vitale P (2018) Fisher metric, geometric entanglement and spin networks. Phys Rev D 97(4):046015. https://doi.org/10.1103/PhysRevD.97.046015 60. Chirco G, Goeßmann A, Oriti D, Zhang M (2020) Group field theory and holographic tensor networks: dynamical corrections to the Ryu-Takayanagi formula. Class Quant Grav 37(9):095011. https://doi.org/10.1088/1361-6382/ab7bb9 61. Chirco G, Oriti D, Zhang M (2018) Ryu-Takayanagi formula for symmetric random tensor networks. Phys Rev D 97(12):126002. https://doi.org/10.1103/PhysRevD.97.126002 62. Chirco G, Oriti D, Zhang M (2018) Group field theory and tensor networks: towards a RyuTakayanagi formula in full quantum gravity. Class Quant Grav 35(11):115011. https://doi.org/ 10.1088/1361-6382/aabf55 63. Colafranceschi E, Oriti D (2021) Quantum gravity states, entanglement graphs and secondquantized tensor networks. JHEP 07:052. https://doi.org/10.1007/JHEP07(2021)052 64. Carrozza S (2016) Flowing in group field theory space: a review. SIGMA 12:070. https://doi. org/10.3842/SIGMA.2016.070 65. Carrozza S, Lahoche V, Oriti D (2017) Renormalizable group field theory beyond melonic diagrams: an example in rank four. Phys Rev D 96(6):066007. https://doi.org/10.1103/PhysRevD. 96.066007 66. Benedetti D, Ben Geloun J, Oriti D (2015) Functional renormalisation group approach for tensorial group field theory: a rank-3 model. JHEP 03:084. https://doi.org/10.1007/ JHEP03(2015)084 67. Dittrich B, Mizera S, Steinhaus S (2016) Decorated tensor network renormalization for lattice gauge theories and spin foam models. New J Phys 18(5):053009 68. Bahr B (2017) On background-independent renormalization of spin foam models. Class Quant Grav 34(7):075001 69. Bahr B, Steinhaus S (2016) Numerical evidence for a phase transition in 4d spin foam quantum gravity. Phys Rev Lett 117(14):141302 70. Oriti D, Sindoni L, Wilson-Ewing E (2016) Emergent Friedmann dynamics with a quantum bounce from quantum gravity condensates. Class Quant Grav 33(22):224001. https://doi.org/ 10.1088/0264-9381/33/22/224001 71. Oriti D (2017) The universe as a quantum gravity condensate. Comptes Rendus Physique 18:235–245. https://doi.org/10.1016/j.crhy.2017.02.003 72. Gielen S, Sindoni L (2016) Quantum cosmology from group field theory condensates: a review. SIGMA 12:082. https://doi.org/10.3842/SIGMA.2016.082 73. Pithis AGA, Sakellariadou M (2019) Group field theory condensate cosmology: an appetizer. Universe 5(6). ISSN 2218-1997. https://doi.org/10.3390/universe5060147. https://www.mdpi. com/2218-1997/5/6/147 74. de Cesare M, Pithis AGA, Sakellariadou M (2016) Cosmological implications of interacting group field theory models: cyclic universe and accelerated expansion. Phys Rev D94(6):064051. https://doi.org/10.1103/PhysRevD.94.064051 75. Takahasi Y, Umezawa H (1975) Thermo field dynamics. Collect Phenom 2:55–80. Reprint https://doi.org/10.1142/S0217979296000817.

180

6 Conclusions

76. Unruh WG (1976) Notes on black hole evaporation. Phys Rev D 14:870. https://doi.org/10. 1103/PhysRevD.14.870 77. Bisognano JJ, Wichmann EH (1976) On the duality condition for quantum fields. J Math Phys 17:303–321. https://doi.org/10.1063/1.522898 78. Hartle JB, Hawking SW (1976) Path integral derivation of black hole radiance. Phys Rev D 13:2188–2203. https://doi.org/10.1103/PhysRevD.13.2188 79. Sewell GL (1982) Quantum fields on manifolds: PCT and gravitationally induced thermal states. Ann Phys 141:201–224. https://doi.org/10.1016/0003-4916(82)90285-8 80. Maldacena JM (2003) Eternal black holes in anti-de Sitter. JHEP 04:021. https://doi.org/10. 1088/1126-6708/2003/04/021 81. Bianchi E, Guglielmon J, Hackl L, Yokomizo N (2016) Squeezed vacua in loop quantum gravity. arXiv:1605.05356 82. Barcelo C, Liberati S, Visser M (2005) Analogue gravity. Living Rev Rel 8:12. https://doi.org/ 10.12942/lrr-2005-12. [Living Rev Rel 14:3 (2011)] 83. Roser P, Valentini A (2014) Classical and quantum cosmology with York time. Class Quant Grav 31(24):245001. https://doi.org/10.1088/0264-9381/31/24/245001 84. Oriti D (2018) Levels of spacetime emergence in quantum gravity. arXiv:1807.04875 85. Oriti D (2014) Disappearance and emergence of space and time in quantum gravity. Stud Hist Phil Sci B46:186–199. https://doi.org/10.1016/j.shpsb.2013.10.006 86. Oriti D (2020) The Bronstein hypercube of quantum gravity. In: Matsubara K, Huggett N, Wüthrich N (eds) Beyond spacetime: the foundations of quantum gravity. Cambridge University Press, Cambridge 87. Montesinos M, Rovelli C (2001) Statistical mechanics of generally covariant quantum theories: a Boltzmann-like approach. Class Quant Grav 18:555–569. https://doi.org/10.1088/02649381/18/3/314 88. Rovelli C (1993) Statistical mechanics of gravity and the thermodynamical origin of time. Class Quant Grav 10:1549–1566. https://doi.org/10.1088/0264-9381/10/8/015 89. Connes A, Rovelli C (1994) Von Neumann algebra automorphisms and time thermodynamics relation in general covariant quantum theories. Class Quant Grav 11:2899–2918. https://doi. org/10.1088/0264-9381/11/12/007 90. Rovelli C (2013) General relativistic statistical mechanics. Phys Rev D 87(8):084055. https:// doi.org/10.1103/PhysRevD.87.084055 91. Chirco G, Haggard HM, Rovelli C (2013) Coupling and thermal equilibrium in generalcovariant systems. Phys Rev D 88:084027. https://doi.org/10.1103/PhysRevD.88.084027 92. Rovelli C, Smerlak M (2011) Thermal time and the Tolman-Ehrenfest effect: temperature as the ‘speed of time’. Class Quant Grav 28:075007. https://doi.org/10.1088/0264-9381/28/7/ 075007 93. Chirco G, Josset T (2016) Statistical mechanics of covariant systems with multi-fingered time. arXiv:1606.04444 94. Kuhn TS (1987) Black-body theory and the quantum discontinuity, 1894-1912. University of Chicago Press 95. Planck M (1909) Eight lectures on theoretical physics. Translation by AP Wills