Xavier Calmet Editor Quantum Aspects of Black Holes Fundamental Theories of Physics
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Models of Phase Stability in Jackiw-Teitelboim Gravity
PHYSICAL REVIEW D 100, 124061 (2019) Models of phase stability in Jackiw-Teitelboim gravity Arindam Lala* Instituto de Física, Pontificia Universidad Católica de Valparaíso, Casilla, 4059 Valparaiso, Chile † Dibakar Roychowdhury Department of Physics, Indian Institute of Technology Roorkee, Roorkee, 247667 Uttarakhand, India (Received 4 October 2019; published 31 December 2019) We construct solutions within Jackiw-Teitelboim (JT) gravity in the presence of nontrivial couplings between the dilaton and the Abelian 1-form where we analyze the asymptotic structure as well as the phase stability corresponding to charged black hole solutions in 1 þ 1 D. We consider the Almheiri-Polchinski model as a specific example within 1 þ 1 D JT gravity which plays a pivotal role in the study of Sachdev-Ye- Kitaev (SYK)/anti–de Sitter (AdS) duality. The corresponding vacuum solutions exhibit a rather different asymptotic structure than their uncharged counterpart. We find interpolating vacuum solutions with AdS2 in the IR and Lifshitz2 in the UV with dynamical exponent zdyn ¼ 3=2. Interestingly, the presence of charge also modifies the black hole geometry from asymptotically AdS to asymptotically Lifshitz with the same value of the dynamical exponent. We consider specific examples, where we compute the corresponding free energy and explore the thermodynamic phase stability associated with charged black hole solutions in 1 þ 1 D. Our analysis reveals the existence of a universal thermodynamic feature that is expected to reveal its immediate consequences on the dual SYK physics at finite density and strong coupling. DOI: 10.1103/PhysRevD.100.124061 I. INTRODUCTION AND MOTIVATIONS For the last couple of years, there has been a systematic For the last couple of decades, there had been consid- effort toward unveiling the dual gravitational counterpart erable efforts toward a profound understanding of the of the SYK model. -
Lecture Notes in Physics
Lecture Notes in Physics Editorial Board R. Beig, Wien, Austria J. Ehlers, Potsdam, Germany U. Frisch, Nice, France K. Hepp, Zurich,¨ Switzerland W. Hillebrandt, Garching, Germany D. Imboden, Zurich,¨ Switzerland R. L. Jaffe, Cambridge, MA, USA R. Kippenhahn, Gottingen,¨ Germany R. Lipowsky, Golm, Germany H. v. Lohneysen,¨ Karlsruhe, Germany I. Ojima, Kyoto, Japan H. A. Weidenmuller,¨ Heidelberg, Germany J. Wess, Munchen,¨ Germany J. Zittartz, Koln,¨ Germany 3 Berlin Heidelberg New York Barcelona Hong Kong London Milan Paris Singapore Tokyo Editorial Policy The series Lecture Notes in Physics (LNP), founded in 1969, reports new developments in physics research and teaching -- quickly, informally but with a high quality. Manuscripts to be considered for publication are topical volumes consisting of a limited number of contributions, carefully edited and closely related to each other. Each contribution should contain at least partly original and previously unpublished material, be written in a clear, pedagogical style and aimed at a broader readership, especially graduate students and nonspecialist researchers wishing to familiarize themselves with the topic concerned. For this reason, traditional proceedings cannot be considered for this series though volumes to appear in this series are often based on material presented at conferences, workshops and schools (in exceptional cases the original papers and/or those not included in the printed book may be added on an accompanying CD ROM, together with the abstracts of posters and other material suitable for publication, e.g. large tables, colour pictures, program codes, etc.). Acceptance Aprojectcanonlybeacceptedtentativelyforpublication,byboththeeditorialboardandthe publisher, following thorough examination of the material submitted. The book proposal sent to the publisher should consist at least of a preliminary table of contents outlining the structureofthebooktogetherwithabstractsofallcontributionstobeincluded. -
The State of the Multiverse: the String Landscape, the Cosmological Constant, and the Arrow of Time
The State of the Multiverse: The String Landscape, the Cosmological Constant, and the Arrow of Time Raphael Bousso Center for Theoretical Physics University of California, Berkeley Stephen Hawking: 70th Birthday Conference Cambridge, 6 January 2011 RB & Polchinski, hep-th/0004134; RB, arXiv:1112.3341 The Cosmological Constant Problem The Landscape of String Theory Cosmology: Eternal inflation and the Multiverse The Observed Arrow of Time The Arrow of Time in Monovacuous Theories A Landscape with Two Vacua A Landscape with Four Vacua The String Landscape Magnitude of contributions to the vacuum energy graviton (a) (b) I Vacuum fluctuations: SUSY cutoff: ! 10−64; Planck scale cutoff: ! 1 I Effective potentials for scalars: Electroweak symmetry breaking lowers Λ by approximately (200 GeV)4 ≈ 10−67. The cosmological constant problem −121 I Each known contribution is much larger than 10 (the observational upper bound on jΛj known for decades) I Different contributions can cancel against each other or against ΛEinstein. I But why would they do so to a precision better than 10−121? Why is the vacuum energy so small? 6= 0 Why is the energy of the vacuum so small, and why is it comparable to the matter density in the present era? Recent observations Supernovae/CMB/ Large Scale Structure: Λ ≈ 0:4 × 10−121 Recent observations Supernovae/CMB/ Large Scale Structure: Λ ≈ 0:4 × 10−121 6= 0 Why is the energy of the vacuum so small, and why is it comparable to the matter density in the present era? The Cosmological Constant Problem The Landscape of String Theory Cosmology: Eternal inflation and the Multiverse The Observed Arrow of Time The Arrow of Time in Monovacuous Theories A Landscape with Two Vacua A Landscape with Four Vacua The String Landscape Many ways to make empty space Topology and combinatorics RB & Polchinski (2000) I A six-dimensional manifold contains hundreds of topological cycles. -
Exact Solutions and Critical Chaos in Dilaton Gravity with a Boundary
Prepared for submission to JHEP INR-TH-2017-002 Exact solutions and critical chaos in dilaton gravity with a boundary Maxim Fitkevicha;b Dmitry Levkova Yegor Zenkevich1c;d;e aInstitute for Nuclear Research of the Russian Academy of Sciences, 60th October An- niversary Prospect 7a, Moscow 117312, Russia bMoscow Institute of Physics and Technology, Institutskii per. 9, Dolgoprudny 141700, Moscow Region, Russia cDipartimento di Fisica, Universit`adi Milano-Bicocca, Piazza della Scienza 3, I-20126 Milano, Italy dINFN, sezione di Milano-Bicocca, I-20126 Milano, Italy eNational Research Nuclear University MEPhI, Moscow 115409, Russia E-mail: [email protected], [email protected], [email protected] Abstract: We consider (1 + 1)-dimensional dilaton gravity with a reflecting dy- namical boundary. The boundary cuts off the region of strong coupling and makes our model causally similar to the spherically-symmetric sector of multidimensional gravity. We demonstrate that this model is exactly solvable at the classical level and possesses an on-shell SL(2; R) symmetry. After introducing general classical solution of the model, we study a large subset of soliton solutions. The latter describe reflec- tion of matter waves off the boundary at low energies and formation of black holes at energies above critical. They can be related to the eigenstates of the auxiliary inte- grable system, the Gaudin spin chain. We argue that despite being exactly solvable, the model in the critical regime, i.e. at the verge of black hole formation, displays arXiv:1702.02576v2 [hep-th] 17 Apr 2017 dynamical instabilities specific to chaotic systems. We believe that this model will be useful for studying black holes and gravitational scattering. -
On Asymptotically De Sitter Space: Entropy & Moduli Dynamics
On Asymptotically de Sitter Space: Entropy & Moduli Dynamics To Appear... [1206.nnnn] Mahdi Torabian International Centre for Theoretical Physics, Trieste String Phenomenology Workshop 2012 Isaac Newton Institute , CAMBRIDGE 1 Tuesday, June 26, 12 WMAP 7-year Cosmological Interpretation 3 TABLE 1 The state of Summarythe ofart the cosmological of Observational parameters of ΛCDM modela Cosmology b c Class Parameter WMAP 7-year ML WMAP+BAO+H0 ML WMAP 7-year Mean WMAP+BAO+H0 Mean 2 +0.056 Primary 100Ωbh 2.227 2.253 2.249−0.057 2.255 ± 0.054 2 Ωch 0.1116 0.1122 0.1120 ± 0.0056 0.1126 ± 0.0036 +0.030 ΩΛ 0.729 0.728 0.727−0.029 0.725 ± 0.016 ns 0.966 0.967 0.967 ± 0.014 0.968 ± 0.012 τ 0.085 0.085 0.088 ± 0.015 0.088 ± 0.014 2 d −9 −9 −9 −9 ∆R(k0) 2.42 × 10 2.42 × 10 (2.43 ± 0.11) × 10 (2.430 ± 0.091) × 10 +0.030 Derived σ8 0.809 0.810 0.811−0.031 0.816 ± 0.024 H0 70.3km/s/Mpc 70.4km/s/Mpc 70.4 ± 2.5km/s/Mpc 70.2 ± 1.4km/s/Mpc Ωb 0.0451 0.0455 0.0455 ± 0.0028 0.0458 ± 0.0016 Ωc 0.226 0.226 0.228 ± 0.027 0.229 ± 0.015 2 +0.0056 Ωmh 0.1338 0.1347 0.1345−0.0055 0.1352 ± 0.0036 e zreion 10.4 10.3 10.6 ± 1.210.6 ± 1.2 f t0 13.79 Gyr 13.76 Gyr 13.77 ± 0.13 Gyr 13.76 ± 0.11 Gyr a The parameters listed here are derived using the RECFAST 1.5 and version 4.1 of the WMAP[WMAP-7likelihood 1001.4538] code. -
University of California Santa Cruz Quantum
UNIVERSITY OF CALIFORNIA SANTA CRUZ QUANTUM GRAVITY AND COSMOLOGY A dissertation submitted in partial satisfaction of the requirements for the degree of DOCTOR OF PHILOSOPHY in PHYSICS by Lorenzo Mannelli September 2005 The Dissertation of Lorenzo Mannelli is approved: Professor Tom Banks, Chair Professor Michael Dine Professor Anthony Aguirre Lisa C. Sloan Vice Provost and Dean of Graduate Studies °c 2005 Lorenzo Mannelli Contents List of Figures vi Abstract vii Dedication viii Acknowledgments ix I The Holographic Principle 1 1 Introduction 2 2 Entropy Bounds for Black Holes 6 2.1 Black Holes Thermodynamics ........................ 6 2.1.1 Area Theorem ............................ 7 2.1.2 No-hair Theorem ........................... 7 2.2 Bekenstein Entropy and the Generalized Second Law ........... 8 2.2.1 Hawking Radiation .......................... 10 2.2.2 Bekenstein Bound: Geroch Process . 12 2.2.3 Spherical Entropy Bound: Susskind Process . 12 2.2.4 Relation to the Bekenstein Bound . 13 3 Degrees of Freedom and Entropy 15 3.1 Degrees of Freedom .............................. 15 3.1.1 Fundamental System ......................... 16 3.2 Complexity According to Local Field Theory . 16 3.3 Complexity According to the Spherical Entropy Bound . 18 3.4 Why Local Field Theory Gives the Wrong Answer . 19 4 The Covariant Entropy Bound 20 4.1 Light-Sheets .................................. 20 iii 4.1.1 The Raychaudhuri Equation .................... 20 4.1.2 Orthogonal Null Hypersurfaces ................... 24 4.1.3 Light-sheet Selection ......................... 26 4.1.4 Light-sheet Termination ....................... 28 4.2 Entropy on a Light-Sheet .......................... 29 4.3 Formulation of the Covariant Entropy Bound . 30 5 Quantum Field Theory in Curved Spacetime 32 5.1 Scalar Field Quantization ......................... -
Page Curve for an Evaporating Black Hole Arxiv:2004.00598V2 [Hep-Th]
Page Curve for an Evaporating Black Hole Friðrik Freyr Gautason?, Lukas Schneiderbauer?, Watse Sybesma? and Lárus Thorlacius? Instituut voor Theoretische Fysica, KU Leuven Celestijnenlaan 200D, 3001 Leuven, Belgium ?Science Institute University of Iceland Dunhaga 3, 107 Reykjavík, Iceland. E-mail: [email protected], [email protected], [email protected], [email protected] Abstract: A Page curve for an evaporating black hole in asymptotically flat spacetime is computed by adapting the Quantum Ryu-Takayanagi (QRT) proposal to an analytically solvable semi-classical two-dimensional dilaton gravity theory. The Page time is found to be one third of the black hole lifetime, at leading order in semi- classical corrections. A Page curve is also obtained for a semi-classical eternal black hole, where energy loss due to Hawking evaporation is balanced by an incoming energy flux. arXiv:2004.00598v2 [hep-th] 21 Apr 2020 Contents 1 Introduction1 2 Page curve from QRT3 3 The model6 3.1 Coupling to matter7 3.2 Semi-classical black holes9 4 Generalized entropy 12 5 Page curves 13 5.1 Eternal black hole 13 5.2 Dynamical black hole 17 5.2.1 Island configuration 17 5.2.2 No-island configuration 20 6 Discussion 20 1 Introduction If black hole evaporation is a unitary process, the entanglement entropy between the outgoing radiation and the quantum state associated to the remaining black hole is expected to follow the so-called Page curve as a function of time [1,2]. Early on, the entanglement entropy is then a monotonically increasing function of time which closely tracks the coarse grained thermal entropy of the radiation that has been emitted up to that point. -
On the Limits of Effective Quantum Field Theory
RUNHETC-2019-15 On the Limits of Effective Quantum Field Theory: Eternal Inflation, Landscapes, and Other Mythical Beasts Tom Banks Department of Physics and NHETC Rutgers University, Piscataway, NJ 08854 E-mail: [email protected] Abstract We recapitulate multiple arguments that Eternal Inflation and the String Landscape are actually part of the Swampland: ideas in Effective Quantum Field Theory that do not have a counterpart in genuine models of Quantum Gravity. 1 Introduction Most of the arguments and results in this paper are old, dating back a decade, and very little of what is written here has not been published previously, or presented in talks. I was motivated to write this note after spending two weeks at the Vacuum Energy and Electroweak Scale workshop at KITP in Santa Barbara. There I found a whole new generation of effective field theorists recycling tired ideas from the 1980s about the use of effective field theory in gravitational contexts. These were ideas that I once believed in, but since the beginning of the 21st century my work in string theory and the dynamics of black holes, convinced me that they arXiv:1910.12817v2 [hep-th] 6 Nov 2019 were wrong. I wrote and lectured about this extensively in the first decade of the century, but apparently those arguments have not been accepted, and effective field theorists have concluded that the main lesson from string theory is that there is a vast landscape of meta-stable states in the theory of quantum gravity, connected by tunneling transitions in the manner envisioned by effective field theorists in the 1980s. -
Geometric Origin of Coincidences and Hierarchies in the Landscape
Geometric origin of coincidences and hierarchies in the landscape The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Bousso, Raphael et al. “Geometric origin of coincidences and hierarchies in the landscape.” Physical Review D 84.8 (2011): n. pag. Web. 26 Jan. 2012. © 2011 American Physical Society As Published http://dx.doi.org/10.1103/PhysRevD.84.083517 Publisher American Physical Society (APS) Version Final published version Citable link http://hdl.handle.net/1721.1/68666 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. PHYSICAL REVIEW D 84, 083517 (2011) Geometric origin of coincidences and hierarchies in the landscape Raphael Bousso,1,2 Ben Freivogel,3 Stefan Leichenauer,1,2 and Vladimir Rosenhaus1,2 1Center for Theoretical Physics and Department of Physics, University of California, Berkeley, California 94720-7300, USA 2Lawrence Berkeley National Laboratory, Berkeley, California 94720-8162, USA 3Center for Theoretical Physics and Laboratory for Nuclear Science, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA (Received 2 August 2011; published 14 October 2011) We show that the geometry of cutoffs on eternal inflation strongly constrains predictions for the time scales of vacuum domination, curvature domination, and observation. We consider three measure proposals: the causal patch, the fat geodesic, and the apparent horizon cutoff, which is introduced here for the first time. We impose neither anthropic requirements nor restrictions on landscape vacua. For vacua with positive cosmological constant, all three measures predict the double coincidence that most observers live at the onset of vacuum domination and just before the onset of curvature domination. -
Arxiv:Hep-Th/0209231 V1 26 Sep 2002 Tbs,Daai N Uigi Eurdfrsae Te Hntetemlvcu Olead to Vacuum Thermal the Anisotropy
SLAC-PUB-9533 BRX TH-505 October 2002 SU-ITP-02/02 Initial conditions for inflation Nemanja Kaloper1;2, Matthew Kleban1, Albion Lawrence1;3;4, Stephen Shenker1 and Leonard Susskind1 1Department of Physics, Stanford University, Stanford, CA 94305 2Department of Physics, University of California, Davis, CA 95616 3Brandeis University Physics Department, MS 057, POB 549110, Waltham, MA 02454y 4SLAC Theory Group, MS 81, 2575 Sand Hill Road, Menlo Park, CA 94025 Free scalar fields in de Sitter space have a one-parameter family of states invariant under the de Sitter group, including the standard thermal vacuum. We show that, except for the thermal vacuum, these states are unphysical when gravitational interactions are arXiv:hep-th/0209231 v1 26 Sep 2002 included. We apply these observations to the quantum state of the inflaton, and find that at best, dramatic fine tuning is required for states other than the thermal vacuum to lead to observable features in the CMBR anisotropy. y Present and permanent address. *Work supported in part by Department of Energy Contract DE-AC03-76SF00515. 1. Introduction In inflationary cosmology, cosmic microwave background (CMB) data place a tanta- lizing upper bound on the vacuum energy density during the inflationary epoch: 4 V M 4 1016 GeV : (1:1) ∼ GUT ∼ Here MGUT is the \unification scale" in supersymmetric grand unified models, as predicted by the running of the observed strong, weak and electromagnetic couplings above 1 T eV in the minimal supersymmetric standard model. If this upper bound is close to the truth, the vacuum energy can be measured directly with detectors sensitive to the polarization of the CMBR. -
A New Look at the RST Model Jian-Ge Zhoua, F. Zimmerschieda, J
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server A new lo ok at the RST mo del a a a,b Jian-Ge Zhou , F. Zimmerschied , J.{Q. Liang and a H. J. W. Muller{Ki rsten a Department of Physics, University of Kaiserslautern, P. O. Box 3049, D{67653 Kaiserslautern, Germany b Institute of Theoretical Physics, Shanxi University Taiyuan, Shanxi 030006, P. R. China and Institute of Physics, Academia Sinica, Beijing 100080, P. R. China Abstract The RST mo del is augmented by the addition of a scalar eld and a b oundary term so that it is well-p osed and lo cal. Expressing the RST action in terms of the ADM formulation, the constraint structure can b e analysed completely.It is shown that from the view p oint of lo cal eld theories, there exists a hidden dynamical eld in the RST mo del. Thanks to the presence of this hidden 1 dynamical eld, we can reconstruct the closed algebra of the constraints which guarantee the general invariance of the RST action. The resulting stress tensors T are recovered to b e true tensor quantities. Esp ecially, the part of the stress tensors for the hidden dynamical eld gives the precise expression for t . 1 At the quantum level, the cancellation condition for the total central charge is reexamined. Finally, with the help of the hidden dynamical eld , the fact 1 that the semi-classical static solution of the RST mo del has two indep endent parameters (P,M), whereas for the classical CGHS mo del there is only one, can b e explained. -
Vavilov-Cherenkov and Synchrotron Radiation Fundamental Theories of Physics
Vavilov-Cherenkov and Synchrotron Radiation Fundamental Theories of Physics An International Book Series on The Fundamental Theories of Physics: Their Clarification, Development and Application Editor: ALWYN VAN DER MERWE, University of Denver, U.S.A. Editorial Advisory Board: GIANCARLO GHIRARDI, University of Trieste, Italy LAWRENCE P. HORWITZ, Tel-Aviv University, Israel BRIAN D. JOSEPHSON, University of Cambridge, U.K. CLIVE KILMISTER, University of London, U.K. PEKKA J. LAHTI, University of Turku, Finland ASHER PERES, Israel Institute of Technology, Israel EDUARD PRUGOVECKI, University of Toronto, Canada FRANCO SELLERI, Università di Bara, Italy TONY SUDBURY, University of York, U.K. HANS-JÜRGEN TREDER, Zentralinstitut für Astrophysik der Akademie der Wissenschaften, Germany Volume 142 Vavilov-Cherenkov and Synchrotron Radiation Foundations and Applications by G.N. Afanasiev Bogoliubov Laboratory of Theoretical Physics, Joint Institute for Nuclear Research, Dubna, Moscow Region, Russia KLUWER ACADEMIC PUBLISHERS NEW YORK, BOSTON, DORDRECHT, LONDON, MOSCOW eBook ISBN: 1-4020-2411-8 Print ISBN: 1-4020-2410-X ©2005 Springer Science + Business Media, Inc. Print ©2004 Kluwer Academic Publishers Dordrecht All rights reserved No part of this eBook may be reproduced or transmitted in any form or by any means, electronic, mechanical, recording, or otherwise, without written consent from the Publisher Created in the United States of America Visit Springer's eBookstore at: http://ebooks.springerlink.com and the Springer Global Website Online at: http://www.springeronline.com CONTENTS PREFACE xi 1 INTRODUCTION 1 2 THE TAMM PROBLEM IN THE VAVILOV-CHERENKOV RADIATION THEORY 15 2.1 Vavilov-Cherenkov radiation in a finite region of space . 15 2.1.1 Mathematicalpreliminaries.............