Holographic Dark Energy Preety Sidhu 5 May 2006. Black Holes and Entropy Black holes are “maximal entropy objects” Entropy of a black hole proportional.

Slides:



Advertisements
Similar presentations
Gerard t Hooft Spinoza Institute, Utrecht University Utrecht University and.
Advertisements

F. Debbasch (LERMA-ERGA Université Paris 6) and M. Bustamante, C. Chevalier, Y. Ollivier Statistical Physics and relativistic gravity ( )
ICHEP conference, Paris, 22/07/10. Emergence Current Paradigm FUNDAMENTAL FORCES: carried by elementary particles.
Black Holes and Particle Species Gia Dvali CERN Theory Division and New York University.
Dark Energy and Quantum Gravity Dark Energy and Quantum Gravity Enikő Regős Enikő Regős.
Finite universe and cosmic coincidences Kari Enqvist, University of Helsinki COSMO 05 Bonn, Germany, August 28 - September 01, 2005.
Astronomy and Cosmologies Spring 2013, Zita Crisis in Cosmology Planck Time Candidate solutions.
The Big Bang Necessary? –Expansion of the Universe –Origin of CMBR 400 photons/cc Black body temperature profile –Helium content Universal nucleosynthesis.
Entropic Gravity SISSA, Statistical Physics JC Friday 28, 2011 E. Verlinde, arXiv: v2 [hep-th]
The Universe’s Acceleration Must Stop If Life Is to Survive Forever Terasem Conference, Vermont July 20, 2005.
Cosmological Structure Formation A Short Course
Gerard ’t Hooft Spinoza Institute Utrecht University CMI, Chennai, 20 November 2009 arXiv:
Quantum Tunneling of Thin Wall Matthew C. Johnson, in collaboration with Anthony Aguirre.
Astronomy and Cosmologies Wed.18.May 2005, last lecture, Spring 2005, Zita Age of the universe – finish H workshop Your questions on Cosmology and the.
Galaxy Evolution 1) Density fluctuations in the primordial matter 2) galaxies grew by repeated merging of smaller objects - evidence: galaxies at large.
Coupled Dark Energy and Dark Matter from dilatation symmetry.
Particle Physics and Cosmology Inflation.
The 2d gravity coupled to a dilaton field with the action This action ( CGHS ) arises in a low-energy asymptotic of string theory models and in certain.
Astronomy and Cosmology week 5 – Tuesday 6 May 2003 LIGHT Star Date Light lecture Workshop: calculate Planck mass (Univ.5e Ch.28) break Minilectures Thursday:
Galileo Galilei Colloquium, Pisa, March 3, 2006 Gerard ’t Hooft Utrecht University.
CERN Colloquium, 28/04/11. Matter and Forces Current Paradigm FUNDAMENTAL FORCES: carried by elementary particles.
Some Conceptual Problems in Cosmology Prof. J. V. Narlikar IUCAA, Pune.
The Quantum Space-Time Juan Maldacena Institute for Advanced Study 25 th Solvay Conference October 2011.
Black Holes Matthew Trimble 10/29/12.
Entropy bounds Introduction Black hole entropy Entropy bounds Holography.
Entropy localization and distribution in the Hawking radiation Horacio Casini CONICET-Intituto Balseiro – Centro Atómico Bariloche.
M ultiverse and the Naturalness Problem Hikaru KAWAI 2012/ 12/ 4 at Osaka University.
Gravitational Wave Backgrounds from Mesoscopic Dynamics of the Extra Dimensions And possibly observable with LIGO, VIRGO, LISA, etc. PRL in press, astro-ph/
Cosmological Reconstruction via Wave Mechanics Peter Coles School of Physics & Astronomy University of Nottingham.
Konstantinos Dimopoulos Lancaster University Contemporary Physics 50 (2009) arXiv: [hep-ph] Invited contribution to 50 th Anniversary.
Announcements The final exam will be at Noon on Monday, December 13 in Van Allen Hall LR1. The final exam will be cumulative. The final will be 40 questions,
Dilaton quantum gravity and cosmology. Dilaton quantum gravity Functional renormalization flow, with truncation :
有效场论、全息原理 暴胀宇宙与暗能量. Effective Field Theory & Holographic Principle An effective field theory that can saturate the equation necessarily includes many.
Studying the equations of the non-linear electrodynamics (NLED) is an attractive subject of research in general relativity. Exact solutions of the Einstein.
DARK ENERGY PARTICLE PHYSICS PROBLEMS STEEN HANNESTAD UNIVERSITY OF AARHUS NBI, 27 AUGUST 2007.
CLOSING THOUGHTS David Gross KITP/UCSB COSMO-02 THANKS Evalyn, John and Sean FOR A CLASSY CONFERENCE.
The false vacuum bubble : - formation and evolution - in collaboration with Chul H. Lee(Hanyang), Wonwoo Lee, Siyong Nam, and Chanyong Park (CQUeST) Based.
Dark Energy Expanding Universe Accelerating Universe Dark Energy Scott Dodelson March 7, 2004.
Holographic and agegraphic dark energy models Yun Soo Myung Inje University, Gimhae, Korea.
10B The Big Bang Where do we come from, where are we going?
Les Houches Lectures on Cosmic Inflation Four Parts 1)Introductory material 2)Entropy, Tuning and Equilibrium in Cosmology 3)Classical and quantum probabilities.
Black holes sourced by a massless scalar KSM2105, FRANKFURT July, 21th 2015 M. Cadoni, University of Cagliari We construct asymptotically flat black hole.
PHY th century cosmology 1920s – 1990s (from Friedmann to Freedman)  theoretical technology available, but no data  20 th century: birth of observational.
Lecture 32: Time’s Arrow Astronomy 1143 Spring 2014.
Inflation, infinity, equilibrium and the observable Universe Andreas Albrecht UC Davis KIPAC Seminar Jan A. Stanford Jan
Composition Until 30 years ago, we thought all matter was “baryonic” matter (protons, neutrons, electrons). Now: 4.6% is baryonic matter 95% is non-baryonic.
Comet Lemmon. AST101 Before the Beginning and other Imponderables.
Holographic Dark Energy and Anthropic Principle Qing-Guo Huang Interdisciplinary Center of Theoretical Studies CAS
Degenerate neutrino as a Dark Energy 12 th Marcel Grossmann Meeting, July 2009, Paris Hyung Won Lee, Inje University July 15, 2009 Collaboration.
KERR BLACK HOLES Generalized BH description includes spin –Later researchers use it to predict new effects!! Two crucial surfaces –inner surface = horizon.
Entanglement in Quantum Gravity and Space-Time Topology
Announcements Final exam is Monday, May 9, at 7:30 am. –Students with last names A-K go to 225 CB. –Students with last names L-Z go to 300 CB. –All students.
Holography, de Sitter space and SUSY breaking Lindefest, Stanford, Mar 7, 2008.
The effect of Gravity on Equation of State Hyeong-Chan Kim (KNUT) FRP Workshop on String Theory and Cosmology 2015, Chungju, Korea, Nov ,
Gravity effects to the Vacuum Bubbles Based on PRD74, (2006), PRD75, (2007), PRD77, (2008), arXiv: [hep-th] & works in preparation.
The Fate of the Universe What property determines the ultimate fate of the universe?
Based on Phys. Rev. D 92, (R) (2015) 中科大交叉学科理论研究中心
Gauge/gravity duality in Einstein-dilaton theory Chanyong Park Workshop on String theory and cosmology (Pusan, ) Ref. S. Kulkarni,
Machian General Relativity A possible solution to the Dark Energy problem and an alternative to Big Bang cosmology ? Robin Booth Theoretical Physics Imperial.
Macroscopic Quantum Geometry Craig Hogan University of Chicago and Fermilab.
Gravity on Matter Equation of State and the Unruh temperature Hyeong-Chan Kim (KNUT) 2016 FRP workshop on String theory and cosmology Seoul, Korea, June.
Causality Problem in Holographic Dark Energy Hyeong-Chan Kim Korea National University of Transportation, with Jungjai Lee (Daejin U.) and Jae-Weon Lee.
Equation of State and Unruh temperature
Formation of universe, blackhole and 1st order phase transition
Solutions of black hole interior, information paradox and the shape of singularities Haolin Lu.
Space-time Invariance and Quantum Gravity
Based on the work submitted to EPJC
Based on Phys. Lett. B 765, 226 (2017) Collaborated with Li You
Quantum gravity predictions for particle physics and cosmology
Presentation transcript:

Holographic Dark Energy Preety Sidhu 5 May 2006

Black Holes and Entropy Black holes are “maximal entropy objects” Entropy of a black hole proportional to surface area of event horizon Max entropy for volume of space goes as bounding surface area, not mass

The Holographic Principle All information about a physical system in some region of space is encoded in its boundary surface, not its volume Like all the information in a room encoded in its walls

Information Entropy Information entropy (or Shannon entropy) measure of “randomness” or “uncertainty” in a signal Thermodynamic entropy like amount of Shannon entropy “missing” between classical macroscopic variables and full microscopic description of system’s state Entropy ultimately measured in bits or nats 1 bit = (ln 2) nats  0.69 nats 1 nat ~ 4 Planck areas Total bits related to matter/energy degrees of freedom Maximum info density, for given volume, about enclosed particle states Matter cannot be infinitely subdivided

Holographic Cosmology Related to the (poorly understood) principles of quantum gravity Bekenstein max entropy for weakly self-gravitating physical system [4D flat spacetime]: S ≤ 2πER Taken to be max holographic entropy for universe

Sizes and Scales In quantum field theory –UV cutoff: short wavelength, high energy bound –IR cutoff: long wavelength, low energy bound –Related by limits set by black hole formation UV limit ~ Planck length IR limit ~ “size of universe” –Particle horizon: largest comoving distance from which light could have reached observer today –Event horizon: largest comoving distance from which light will ever reach observer

Vacuum Fluctuations Uncertainty principle for quantum vacuum energy fluctuations, with N degrees of freedom Holographic principle sets N within UV and IR cutoffs One degree of freedom is a maximum entropy of one Boltzmann unit k Corresponds to Ω = π/4  (z) = -1+(1- π/4)z No adjustable parameters, consistent with recent cosmological observations

Holographic Bounds Holographic entropy bound violated for closed universe of particle horizon size Can solve for closed universe: –Replace particle horizon with event horizon –Add negative pressure component –Or Hubble scale IR cutoff with non-minimal coupling to scalar field