Vacuum energy, cosmological constant problem and the worst theoretical prediction ever

Size: px
Start display at page:

Download "Vacuum energy, cosmological constant problem and the worst theoretical prediction ever"

Transcription

1 Vacuum energy, cosmological constant problem and the worst theoretical prediction ever Juraj Tekel Student Perspectives in Physics, Graduate Center CUNY 3/25/2011

2 Ground state of quantum harmonic oscillator has energy E = 1 2 ω Quantum field is equivalent to collection of harmonic oscillators with ω k = k 2 + m 2 So the ground state has energy density ρ = d 3 k (2π) ω k

3 After regularization, this is proportional to with ε the cutoff distance. ρ ε 4 And with some nice story this is usually discarded... however...

4 The stories do not work if we work in curved space-time. Here the action is S = d 4 x gl(φ, φ) and constant shift in energy is no longer a constant term in the action. It effects equations of motion for the metric itself.

5 For the Einstein-Hilbert action S = d 4 x [ ] 1 g R + L(φ, φ) 16πG we get equations of motion for the space-time metric R µν 1 2 g µνr + 8πG ρ g µν = 8πGT µν So the vacuum energy is equivalent to a cosmological constant.

6 Indeed the most general action S = d 4 x [ ] 1 g 16πG (R 2Λ 0) + L(φ, φ) Gives equations R µν 1 2 g µνr + Λg µν = 8πG With an effective cosmological constant Λ = Λ 0 + 8πGρ

7 So where is the problem?

8 Cosmological constant matter has some very peculiar properties energy-momentum tensor and thus negative pressure T µν = Λ 8πG g µν the energy density is constant repulsive gravity Plus all observations were compatible with the assumption Λ = 0, so nobody really cared... however...

9 We now believe that the universe has positive cosmological constant, because the expansion of universe is accelerating (distant supernovae) repulsive gravity of Λ the universe is flat (CMB anisotropies) but baryons and dark matter make only 30% of critical density

10 So where is the problem? Vacuum energy TRULY IS the cosmological constant. Problem solved... however...

11 To predict the value, we take the cutoff to be Plank length and get the corresponding energy density ρ GeV 4 Value of the cosmological constant energy density consistent with the measurements is ρ GeV 4

12 The difference is 118 ORDERS OF MAGNITUDE!!!

13 And nobody really knows what to do now. Supersymmetry? Supergravity and Superstrings? Antropic principle? Different source of dark energy? etc. All the solutions to the problem require enormous fine tuning. As of now, no physical principle is know that requires Λ to be so small.

14 What do we have to say about this?

15 We do not offer a solution. We rather claim that the problem is ill defined from the very beginning.

16 Vacuum fluctuations in curved space can produce configurations, that create black holes. Such fluctuations would make the vacuum unstable, showing that we can not combine quantum fields and general relativity just like that. We try to compute rate, at which black holes occur in vacuum.

17 In vacuum 0 the probability distribution for any observable A is P(α)dα = 0 δ (α A) 0 dα This yields αp(α)dα = ᾱ = 0 A 0 α 2 P(α)dα = ᾱ2 = 0 A 2 0

18 Probability, that we will find energy in interval E, E + de in volume V as a result of fluctuation in vacuum is therefor ( ) P(E, V )de = 0 δ E T 00 (x)d 3 x 0 de If the energy inside volume V is greater than 3 V, this region will collapse into a black hole. We convert the probability into rate by assuming, that the sample time is proportional to the light travel time across the volume V. V

19 Seems rather random, but this choice is well motivated the only meaningful time in the problem information about rearrangement cross-section formula for black hole formation and particles colliding in V

20 For the probability, we get Gaussian distribution P(E, V )de = 1 2πσ 2 (E µ)2 e 2σ 2 de with µ = σ 2 = V V d 3 x 0 T 00 (x) 0 d 3 xd 3 y 0 T 00 (x)t 00 (y) 0 Note that the first integral reproduces the formula for the vacuum energy from the first slide. Indeed, up to the first order P(E, V )de = δ(e µ)de

21 Some technicalities We work with a simple theory of a massless scalar field. We regulate the momentum integrals by introducing d 3 k d 3 ke ε k and later setting ε to be the Plank length. We also take the volume V to be a sphere.

22 The final formula for the total rate is R = 6 1/6 5 1/2 π 5/6 ε 2 ε de 1 5π 4/3 (3E 2 π 2 ε 4 ) 2 e 6 1/3 ε 4 E 7/3 The problem is that this gives rates much higher than expected. So far seems to give results around black holes every second in very cm 3.

23 Well, we still work on that. Thanks for your attention!

Generalized Wigner distributions and scalar field on a fuzzy sphere

Generalized Wigner distributions and scalar field on a fuzzy sphere Generalized Wigner distributions and scalar field on a fuzzy sphere Juraj Tekel The Graduate Center and The City College The City University of New York work with V.P. Nair and A. Polychronakos Models

More information

The Cosmological Principle

The Cosmological Principle Cosmological Models John O Byrne School of Physics University of Sydney Using diagrams and pp slides from Seeds Foundations of Astronomy and the Supernova Cosmology Project http://www-supernova.lbl.gov

More information

Set 3: Cosmic Dynamics

Set 3: Cosmic Dynamics Set 3: Cosmic Dynamics FRW Dynamics This is as far as we can go on FRW geometry alone - we still need to know how the scale factor a(t) evolves given matter-energy content General relativity: matter tells

More information

Galaxy Formation Seminar 2: Cosmological Structure Formation as Initial Conditions for Galaxy Formation. Prof. Eric Gawiser

Galaxy Formation Seminar 2: Cosmological Structure Formation as Initial Conditions for Galaxy Formation. Prof. Eric Gawiser Galaxy Formation Seminar 2: Cosmological Structure Formation as Initial Conditions for Galaxy Formation Prof. Eric Gawiser Cosmic Microwave Background anisotropy and Large-scale structure Cosmic Microwave

More information

THE DARK SIDE OF THE COSMOLOGICAL CONSTANT

THE DARK SIDE OF THE COSMOLOGICAL CONSTANT THE DARK SIDE OF THE COSMOLOGICAL CONSTANT CAMILO POSADA AGUIRRE University of South Carolina Department of Physics and Astronomy 09/23/11 Outline 1 Einstein s Greatest Blunder 2 The FLRW Universe 3 A

More information

Theoretical Explanations for Cosmic Acceleration

Theoretical Explanations for Cosmic Acceleration Theoretical Explanations for Cosmic Acceleration Eanna Flanagan, Cornell Physics Colloquium, University of Guelph, 17 October 2006 Outline Recent observations show that the expansion of the Universe is

More information

Ta-Pei Cheng PCNY 9/16/2011

Ta-Pei Cheng PCNY 9/16/2011 PCNY 9/16/2011 Ta-Pei Cheng For a more quantitative discussion, see Relativity, Gravitation & Cosmology: A Basic Introduction (Oxford Univ Press) 2 nd ed. (2010) dark matter & dark energy Astronomical

More information

The Cosmological Constant Problem

The Cosmological Constant Problem Physics 171 Fall 2015 The Cosmological Constant Problem 1 The numerical value of the vacuum energy density The cosmological constant Λ was introduced by Albert Einstein into general relativity in 1917

More information

One of the problems in modern physics

One of the problems in modern physics The Cosmological Constant One of the problems in modern physics Hendrik van Hees Fakultät für Physik Universität Bielefeld The Cosmological Constant p.1 Contents Fundamentals from General relativity: The

More information

Effect of the Trace Anomaly on the Cosmological Constant. Jurjen F. Koksma

Effect of the Trace Anomaly on the Cosmological Constant. Jurjen F. Koksma Effect of the Trace Anomaly on the Cosmological Constant Jurjen F. Koksma Invisible Universe Spinoza Institute Institute for Theoretical Physics Utrecht University 2nd of July 2009 J.F. Koksma T. Prokopec

More information

New Blackhole Theorem and its Applications to Cosmology and Astrophysics

New Blackhole Theorem and its Applications to Cosmology and Astrophysics New Blackhole Theorem and its Applications to Cosmology and Astrophysics I. New Blackhole Theorem II. Structure of the Universe III. New Law of Gravity IV. PID-Cosmological Model Tian Ma, Shouhong Wang

More information

Cosmology Dark Energy Models ASTR 2120 Sarazin

Cosmology Dark Energy Models ASTR 2120 Sarazin Cosmology Dark Energy Models ASTR 2120 Sarazin Late Homeworks Last day Wednesday, May 1 My mail box in ASTR 204 Maximum credit 50% unless excused (but, better than nothing) Final Exam Thursday, May 2,

More information

General Relativity Lecture 20

General Relativity Lecture 20 General Relativity Lecture 20 1 General relativity General relativity is the classical (not quantum mechanical) theory of gravitation. As the gravitational interaction is a result of the structure of space-time,

More information

Lecture 12. Inflation. What causes inflation. Horizon problem Flatness problem Monopole problem. Physical Cosmology 2011/2012

Lecture 12. Inflation. What causes inflation. Horizon problem Flatness problem Monopole problem. Physical Cosmology 2011/2012 Lecture 1 Inflation Horizon problem Flatness problem Monopole problem What causes inflation Physical Cosmology 11/1 Inflation What is inflation good for? Inflation solves 1. horizon problem. flatness problem

More information

Critical exponents in quantum Einstein gravity

Critical exponents in quantum Einstein gravity Critical exponents in quantum Einstein gravity Sándor Nagy Department of Theoretical physics, University of Debrecen MTA-DE Particle Physics Research Group, Debrecen Leibnitz, 28 June Critical exponents

More information

Cosmology (Cont.) Lecture 19

Cosmology (Cont.) Lecture 19 Cosmology (Cont.) Lecture 19 1 General relativity General relativity is the classical theory of gravitation, and as the gravitational interaction is due to the structure of space-time, the mathematical

More information

Quantum Fields in Curved Spacetime

Quantum Fields in Curved Spacetime Quantum Fields in Curved Spacetime Lecture 3 Finn Larsen Michigan Center for Theoretical Physics Yerevan, August 22, 2016. Recap AdS 3 is an instructive application of quantum fields in curved space. The

More information

Potential Discoveries at the Large Hadron Collider. Chris Quigg

Potential Discoveries at the Large Hadron Collider. Chris Quigg Potential Discoveries at the Large Hadron Collider Chris Quigg Fermilab quigg@fnal.gov XXIII Taiwan Spring School Tainan 31 March - 3 April 2010 Electroweak theory successes Theoretical Physics Department,

More information

The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004

The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004 The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004 The history of modern cosmology 1917 Static via cosmological constant? (Einstein) 1917 Expansion (Slipher) 1952 Big Bang criticism (Hoyle)

More information

The Unifying Dark Fluid Model

The Unifying Dark Fluid Model The Model Centre de Recherche Astrophysique de Lyon Invisible Universe Paris July 2nd, 2009 s Dark Matter Problem Dark Matter Dark Energy Dark Fluids? Different scales involved Galactic scale Galaxy Rotation

More information

Law of Gravity and Gravitational Radiation

Law of Gravity and Gravitational Radiation Law of Gravity and Gravitational Radiation Tian Ma, Shouhong Wang Supported in part by NSF and ONR http://www.indiana.edu/ fluid Blog: https://physicalprinciples.wordpress.com I. Laws of Gravity, Dark

More information

Cosmology: An Introduction. Eung Jin Chun

Cosmology: An Introduction. Eung Jin Chun Cosmology: An Introduction Eung Jin Chun Cosmology Hot Big Bang + Inflation. Theory of the evolution of the Universe described by General relativity (spacetime) Thermodynamics, Particle/nuclear physics

More information

Dark Energy vs. Dark Matter: Towards a unifying scalar field?

Dark Energy vs. Dark Matter: Towards a unifying scalar field? Dark Energy vs. Dark Matter: Towards a unifying scalar field? Alexandre ARBEY Centre de Recherche Astrophysique de Lyon Institut de Physique Nucléaire de Lyon, March 2nd, 2007. Introduction The Dark Stuff

More information

The early and late time acceleration of the Universe

The early and late time acceleration of the Universe The early and late time acceleration of the Universe Tomo Takahashi (Saga University) March 7, 2016 New Generation Quantum Theory -Particle Physics, Cosmology, and Chemistry- @Kyoto University The early

More information

Cosmic Inflation Lecture 16 - Monday Mar 10

Cosmic Inflation Lecture 16 - Monday Mar 10 Physics 224 Spring 2008 Origin and Evolution of the Universe Cosmic Inflation Lecture 16 - Monday Mar 10 Joel Primack University of California, Santa Cruz Outline L15 L16 WMAP 5-year Data and Papers Released

More information

In Quest of a True Model of the Universe 1

In Quest of a True Model of the Universe 1 In Quest of a True Model of the Universe 1 R. G. Vishwakarma arxiv:astro-ph/0404371v2 15 May 2004 Department of Mathematics Autonomous University of Zacatecas Zacatecas, ZAC C.P. 98060 Mexico Email: rvishwa@mate.reduaz.mx

More information

Cosmic Bubble Collisions

Cosmic Bubble Collisions Outline Background Expanding Universe: Einstein s Eqn with FRW metric Inflationary Cosmology: model with scalar field QFTà Bubble nucleationà Bubble collisions Bubble Collisions in Single Field Theory

More information

Triple unification of inflation, dark matter and dark energy

Triple unification of inflation, dark matter and dark energy Triple unification of inflation, dark matter and dark energy May 9, 2008 Leonard Susskind, The Anthropic Landscape of String Theory (2003) A. Liddle, A. Ureña-López, Inflation, dark matter and dark energy

More information

Cosmological constant is a conserved charge

Cosmological constant is a conserved charge Cosmological constant is a conserved Kamal Hajian Institute for Research in Fundamental Sciences (IPM) In collaboration with Dmitry Chernyavsky (Tomsk Polytechnic U.) arxiv:1710.07904, to appear in Classical

More information

What do we really know about Dark Energy?

What do we really know about Dark Energy? What do we really know about Dark Energy? Ruth Durrer Département de Physique Théorique & Center of Astroparticle Physics (CAP) ESTEC, February 3, 2012 Ruth Durrer (Université de Genève ) Dark Energy ESTEC

More information

The Effects of Inhomogeneities on the Universe Today. Antonio Riotto INFN, Padova

The Effects of Inhomogeneities on the Universe Today. Antonio Riotto INFN, Padova The Effects of Inhomogeneities on the Universe Today Antonio Riotto INFN, Padova Frascati, November the 19th 2004 Plan of the talk Short introduction to Inflation Short introduction to cosmological perturbations

More information

and Zoran Rakić Nonlocal modified gravity Ivan Dimitrijević, Branko Dragovich, Jelena Grujić

and Zoran Rakić Nonlocal modified gravity Ivan Dimitrijević, Branko Dragovich, Jelena Grujić Motivation Large cosmological observational findings: High orbital speeds of galaxies in clusters.( F.Zwicky, 1933) High orbital speeds of stars in spiral galaxies. ( Vera Rubin, at the end of 1960es )

More information

Chapter 4. COSMOLOGICAL PERTURBATION THEORY

Chapter 4. COSMOLOGICAL PERTURBATION THEORY Chapter 4. COSMOLOGICAL PERTURBATION THEORY 4.1. NEWTONIAN PERTURBATION THEORY Newtonian gravity is an adequate description on small scales (< H 1 ) and for non-relativistic matter (CDM + baryons after

More information

The Theory of Inflationary Perturbations

The Theory of Inflationary Perturbations The Theory of Inflationary Perturbations Jérôme Martin Institut d Astrophysique de Paris (IAP) Indian Institute of Technology, Chennai 03/02/2012 1 Introduction Outline A brief description of inflation

More information

PHY326/426:Lecture 19

PHY326/426:Lecture 19 PHY326/426:Lecture 19 Dark Energy Finish WIMP signals Evidence for Dark Energy Type Ia Supernovae What is Dark Energy The fate of the Universe The Distance-Redshift relation Recall from lecture 2: The

More information

κ = f (r 0 ) k µ µ k ν = κk ν (5)

κ = f (r 0 ) k µ µ k ν = κk ν (5) 1. Horizon regularity and surface gravity Consider a static, spherically symmetric metric of the form where f(r) vanishes at r = r 0 linearly, and g(r 0 ) 0. Show that near r = r 0 the metric is approximately

More information

Relativity, Gravitation, and Cosmology

Relativity, Gravitation, and Cosmology Relativity, Gravitation, and Cosmology A basic introduction TA-PEI CHENG University of Missouri St. Louis OXFORD UNIVERSITY PRESS Contents Parti RELATIVITY Metric Description of Spacetime 1 Introduction

More information

Introduction to Inflation

Introduction to Inflation Introduction to Inflation Miguel Campos MPI für Kernphysik & Heidelberg Universität September 23, 2014 Index (Brief) historic background The Cosmological Principle Big-bang puzzles Flatness Horizons Monopoles

More information

Cosmological Tests of Gravity

Cosmological Tests of Gravity Cosmological Tests of Gravity Levon Pogosian Simon Fraser University, Canada VIA Lecture, 16 May, 2014 Workshop on Testing Gravity at SFU Harbour Centre January 15-17, 2015 Alternative theories of gravity

More information

Holographic Space Time

Holographic Space Time Holographic Space Time Tom Banks (work with W.Fischler) April 1, 2015 The Key Points General Relativity as Hydrodynamics of the Area Law - Jacobson The Covariant Entropy/Holographic Principle - t Hooft,

More information

Holographic Cosmological Constant and Dark Energy arxiv: v1 [hep-th] 16 Sep 2007

Holographic Cosmological Constant and Dark Energy arxiv: v1 [hep-th] 16 Sep 2007 Holographic Cosmological Constant and Dark Energy arxiv:0709.2456v1 [hep-th] 16 Sep 2007 Chao-Jun Feng Institute of Theoretical Physics, Academia Sinica Beijing 100080, China fengcj@itp.ac.cn A general

More information

Inflation Scheme Derived from Universal Wave Function Interpretation of String Theory

Inflation Scheme Derived from Universal Wave Function Interpretation of String Theory Journal of Physical Science and Application 7 (4) (2017) 33-37 doi: 10.17265/2159-5348/2017.04.004 D DAVID PUBLISHING Inflation Scheme Derived from Universal Wave Function Interpretation of String Theory

More information

The cosmological constant puzzle

The cosmological constant puzzle The cosmological constant puzzle Steven Bass Cosmological constant puzzle: Accelerating Universe: believed to be driven by energy of nothing (vacuum) Vacuum energy density (cosmological constant or dark

More information

4 Evolution of density perturbations

4 Evolution of density perturbations Spring term 2014: Dark Matter lecture 3/9 Torsten Bringmann (torsten.bringmann@fys.uio.no) reading: Weinberg, chapters 5-8 4 Evolution of density perturbations 4.1 Statistical description The cosmological

More information

El Universo en Expansion. Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004

El Universo en Expansion. Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004 El Universo en Expansion Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004 5 billion years (you are here) Space is Homogeneous and Isotropic General Relativity An Expanding Universe

More information

Constraining Modified Gravity and Coupled Dark Energy with Future Observations Matteo Martinelli

Constraining Modified Gravity and Coupled Dark Energy with Future Observations Matteo Martinelli Coupled Dark University of Rome La Sapienza Roma, October 28th 2011 Outline 1 2 3 4 5 1 2 3 4 5 Accelerated Expansion Cosmological data agree with an accelerated expansion of the Universe d L [Mpc] 16000

More information

Braneworlds: gravity & cosmology. David Langlois APC & IAP, Paris

Braneworlds: gravity & cosmology. David Langlois APC & IAP, Paris Braneworlds: gravity & cosmology David Langlois APC & IAP, Paris Outline Introduction Extra dimensions and gravity Large (flat) extra dimensions Warped extra dimensions Homogeneous brane cosmology Brane

More information

From inflation to the CMB to today s universe. I - How it all begins

From inflation to the CMB to today s universe. I - How it all begins From inflation to the CMB to today s universe I - How it all begins Raul Abramo Physics Institute - University of São Paulo abramo@fma.if.usp.br redshift Very brief cosmic history 10 9 200 s BBN 1 MeV

More information

Experimental Tests and Alternative Theories of Gravity

Experimental Tests and Alternative Theories of Gravity Experimental Tests and Alternative Theories of Gravity Gonzalo J. Olmo Alba gonzalo.olmo@uv.es University of Valencia (Spain) & UW-Milwaukee Experimental Tests and Alternative Theories of Gravity p. 1/2

More information

Is Cosmic Acceleration Telling Us Something About Gravity?

Is Cosmic Acceleration Telling Us Something About Gravity? Is Cosmic Acceleration Telling Us Something About Gravity? Mark Trodden Syracuse University [See many other talks at this meeting; particularly talks by Carroll, Dvali, Deffayet,... ] NASA Meeting: From

More information

XIII. The Very Early Universe and Inflation. ASTR378 Cosmology : XIII. The Very Early Universe and Inflation 171

XIII. The Very Early Universe and Inflation. ASTR378 Cosmology : XIII. The Very Early Universe and Inflation 171 XIII. The Very Early Universe and Inflation ASTR378 Cosmology : XIII. The Very Early Universe and Inflation 171 Problems with the Big Bang The Flatness Problem The Horizon Problem The Monopole (Relic Particle)

More information

The Expanding Universe

The Expanding Universe Cosmology Expanding Universe History of the Universe Cosmic Background Radiation The Cosmological Principle Cosmology and General Relativity Dark Matter and Dark Energy Primitive Cosmology If the universe

More information

From Inflation to TeV physics: Higgs Reheating in RG Improved Cosmology

From Inflation to TeV physics: Higgs Reheating in RG Improved Cosmology From Inflation to TeV physics: Higgs Reheating in RG Improved Cosmology Yi-Fu Cai June 18, 2013 in Hefei CYF, Chang, Chen, Easson & Qiu, 1304.6938 Two Standard Models Cosmology CMB: Cobe (1989), WMAP (2001),

More information

Arvind Borde / MTH 675, Unit 20: Cosmology

Arvind Borde / MTH 675, Unit 20: Cosmology Arvind Borde / MTH 675, Unit 20: Cosmology 1. Review (1) What do we do when we do GR? We try to solve Einstein s equation. (2) What is Einstein s equation? and R ab = e[ 1 2 ged ( a g bd + b g ad d g ab

More information

The Cosmological Constant and its Interpretation Andrew Liddle. Encyclopedia of Astronomy & Astrophysics P. Murdin

The Cosmological Constant and its Interpretation Andrew Liddle. Encyclopedia of Astronomy & Astrophysics P. Murdin eaa.iop.org DOI: 10.1888/0333750888/2125 The Cosmological Constant and its Interpretation Andrew Liddle From Encyclopedia of Astronomy & Astrophysics P. Murdin IOP Publishing Ltd 2006 ISBN: 0333750888

More information

Cosmological perturbations in f(r) theories

Cosmological perturbations in f(r) theories 5 th IBERIAN COSMOLOGY MEETING 30 th March 2010, Porto, Portugal Cosmological perturbations in f(r) theories Álvaro de la Cruz-Dombriz Theoretical Physics Department Complutense University of Madrid in

More information

Lecture 13 Friedmann Model

Lecture 13 Friedmann Model Lecture 13 Friedmann Model FRW Model for the Einstein Equations First Solutions Einstein (Static Universe) de Sitter (Empty Universe) and H(t) Steady-State Solution (Continuous Creation of Matter) Friedmann-Lemaître

More information

Effective Field Theory in Cosmology

Effective Field Theory in Cosmology C.P. Burgess Effective Field Theory in Cosmology Clues for cosmology from fundamental physics Outline Motivation and Overview Effective field theories throughout physics Decoupling and naturalness issues

More information

Cosmology ASTR 2120 Sarazin. Hubble Ultra-Deep Field

Cosmology ASTR 2120 Sarazin. Hubble Ultra-Deep Field Cosmology ASTR 2120 Sarazin Hubble Ultra-Deep Field Cosmology - Da Facts! 1) Big Universe of Galaxies 2) Sky is Dark at Night 3) Isotropy of Universe Cosmological Principle = Universe Homogeneous 4) Hubble

More information

Quintessence - a fifth force from variation of the fundamental scale

Quintessence - a fifth force from variation of the fundamental scale Quintessence - a fifth force from variation of the fundamental scale Ω m + X = 1? Ω m : 25% Ω h : 75% Dark Energy Quintessence C.Wetterich A.Hebecker,M.Doran,M.Lilley,J.Schwindt, C.Müller,G.Sch ller,g.schäfer,e.thommes,

More information

Cosmic Background Radiation

Cosmic Background Radiation Cosmic Background Radiation The Big Bang generated photons, which scattered frequently in the very early Universe, which was opaque. Once recombination happened the photons are scattered one final time

More information

Inflation and the cosmological constant problem

Inflation and the cosmological constant problem Inflation and the cosmological constant problem Larissa Lorenz Sebastian Sapeta Krzyzowa 18. 8. September 00 Contents Standard model of cosmology and its problems The inflationary paradigm Review of the

More information

Nonparametric Inference and the Dark Energy Equation of State

Nonparametric Inference and the Dark Energy Equation of State Nonparametric Inference and the Dark Energy Equation of State Christopher R. Genovese Peter E. Freeman Larry Wasserman Department of Statistics Carnegie Mellon University http://www.stat.cmu.edu/ ~ genovese/

More information

Dark Matter and Dark Energy

Dark Matter and Dark Energy Dark Matter and Dark Energy Sean Carroll, University of Chicago Our universe, as inventoried over the last ten years: 5% Ordinary Matter 25% D ark M atter 70% Dark Energy Dark Energy Dark Matter Ordinary

More information

Dark Universe II. The shape of the Universe. The fate of the Universe. Old view: Density of the Universe determines its destiny

Dark Universe II. The shape of the Universe. The fate of the Universe. Old view: Density of the Universe determines its destiny Dark Universe II Prof. Lynn Cominsky Dept. of Physics and Astronomy Sonoma State University Modifications by H. Geller November 2007 11/27/2007 Prof. Lynn Cominsky 2 Dark Energy and the Shape of the Universe

More information

Coupled Dark Energy and Dark Matter from dilatation symmetry

Coupled Dark Energy and Dark Matter from dilatation symmetry Coupled Dark Energy and Dark Matter from dilatation symmetry Cosmological Constant - Einstein - Constant λ compatible with all symmetries Constant λ compatible with all observations No time variation in

More information

Inflation and the origin of structure in the Universe

Inflation and the origin of structure in the Universe Phi in the Sky, Porto 0 th July 004 Inflation and the origin of structure in the Universe David Wands Institute of Cosmology and Gravitation University of Portsmouth outline! motivation! the Primordial

More information

Lecture 05. Cosmology. Part I

Lecture 05. Cosmology. Part I Cosmology Part I What is Cosmology Cosmology is the study of the universe as a whole It asks the biggest questions in nature What is the content of the universe: Today? Long ago? In the far future? How

More information

Dark Energy: Back to Newton? Lucy Calder and Ofer Lahav University College London

Dark Energy: Back to Newton? Lucy Calder and Ofer Lahav University College London Dark Energy: Back to Newton? Lucy Calder and Ofer Lahav University College London Key Points of the Paper The original concept by Newton and Hooke in the 17 th century Inverse square law plus a force of

More information

Lecture 1 General relativity and cosmology. Kerson Huang MIT & IAS, NTU

Lecture 1 General relativity and cosmology. Kerson Huang MIT & IAS, NTU A Superfluid Universe Lecture 1 General relativity and cosmology Kerson Huang MIT & IAS, NTU Lecture 1. General relativity and cosmology Mathematics and physics Big bang Dark energy Dark matter Robertson-Walker

More information

Cosmology and the origin of structure

Cosmology and the origin of structure 1 Cosmology and the origin of structure ocy I: The universe observed ocy II: Perturbations ocy III: Inflation Primordial perturbations CB: a snapshot of the universe 38, AB correlations on scales 38, light

More information

Observational evidence and cosmological constant. Kazuya Koyama University of Portsmouth

Observational evidence and cosmological constant. Kazuya Koyama University of Portsmouth Observational evidence and cosmological constant Kazuya Koyama University of Portsmouth Basic assumptions (1) Isotropy and homogeneity Isotropy CMB fluctuation ESA Planck T 5 10 T Homogeneity galaxy distribution

More information

The Friedmann Equation R = GM R 2. R(t) R R = GM R GM R. d dt. = d dt 1 2 R 2 = GM R + K. Kinetic + potential energy per unit mass = constant

The Friedmann Equation R = GM R 2. R(t) R R = GM R GM R. d dt. = d dt 1 2 R 2 = GM R + K. Kinetic + potential energy per unit mass = constant The Friedmann Equation R = GM R R R = GM R R R(t) d dt 1 R = d dt GM R M 1 R = GM R + K Kinetic + potential energy per unit mass = constant The Friedmann Equation 1 R = GM R + K M = ρ 4 3 π R3 1 R = 4πGρR

More information

Astronomy 182: Origin and Evolution of the Universe

Astronomy 182: Origin and Evolution of the Universe Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 14 Dec. 2, 2015 Today The Inflationary Universe Origin of Density Perturbations Gravitational Waves Origin and Evolution of

More information

Chapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc.

Chapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc. Chapter 23 Lecture The Cosmic Perspective Seventh Edition Dark Matter, Dark Energy, and the Fate of the Universe Curvature of the Universe The Density Parameter of the Universe Ω 0 is defined as the ratio

More information

A brain teaser: The anthropic principle! Last lecture I said Is cosmology a science given that we only have one Universe? Weak anthropic principle: "T

A brain teaser: The anthropic principle! Last lecture I said Is cosmology a science given that we only have one Universe? Weak anthropic principle: T Observational cosmology: The Friedman equations 1 Filipe B. Abdalla Kathleen Lonsdale Building G.22 http://zuserver2.star.ucl.ac.uk/~hiranya/phas3136/phas3136 A brain teaser: The anthropic principle! Last

More information

Gravitation et Cosmologie: le Modèle Standard Cours 8: 6 fevrier 2009

Gravitation et Cosmologie: le Modèle Standard Cours 8: 6 fevrier 2009 Particules Élémentaires, Gravitation et Cosmologie Année 2008-09 Gravitation et Cosmologie: le Modèle Standard Cours 8: 6 fevrier 2009 Le paradigme inflationnaire Homogeneity and flatness problems in HBB

More information

The Once and Future CMB

The Once and Future CMB The Once and Future CMB DOE, Jan. 2002 Wayne Hu The On(c)e Ring Original Power Spectra of Maps 64º Band Filtered Ringing in the New Cosmology Gravitational Ringing Potential wells = inflationary seeds

More information

BRANE COSMOLOGY and Randall-Sundrum model

BRANE COSMOLOGY and Randall-Sundrum model BRANE COSMOLOGY and Randall-Sundrum model M. J. Guzmán June 16, 2009 Standard Model of Cosmology CMB and large-scale structure observations provide us a high-precision estimation of the cosmological parameters:

More information

MASAHIDE YAMAGUCHI. Quantum generation of density perturbations in the early Universe. (Tokyo Institute of Technology)

MASAHIDE YAMAGUCHI. Quantum generation of density perturbations in the early Universe. (Tokyo Institute of Technology) Quantum generation of density perturbations in the early Universe MASAHIDE YAMAGUCHI (Tokyo Institute of Technology) 03/07/16@Symposium: New Generation Quantum Theory -Particle Physics, Cosmology, and

More information

Theory of galaxy formation

Theory of galaxy formation Theory of galaxy formation Bibliography: Galaxy Formation and Evolution (Mo, van den Bosch, White 2011) Lectures given by Frank van den Bosch in Yale http://www.astro.yale.edu/vdbosch/teaching.html Theory

More information

Olbers Paradox. Lecture 14: Cosmology. Resolutions of Olbers paradox. Cosmic redshift

Olbers Paradox. Lecture 14: Cosmology. Resolutions of Olbers paradox. Cosmic redshift Lecture 14: Cosmology Olbers paradox Redshift and the expansion of the Universe The Cosmological Principle Ω and the curvature of space The Big Bang model Primordial nucleosynthesis The Cosmic Microwave

More information

What is the Universe Made Of?

What is the Universe Made Of? What is the Universe Made Of? The case for Dark Matter and Dark Energy, and for what they might be Cliff Burgess What is the Universe Made Of? From best fits to the Concordance Cosmology Courtesy: Ned

More information

From Quantum Mechanics to String Theory

From Quantum Mechanics to String Theory From Quantum Mechanics to String Theory Relativity (why it makes sense) Quantum mechanics: measurements and uncertainty Smashing things together: from Rutherford to the LHC Particle Interactions Quarks

More information

with Matter and Radiation By: Michael Solway

with Matter and Radiation By: Michael Solway Interactions of Dark Energy with Matter and Radiation By: Michael Solway Advisor: Professor Mike Berger What is Dark Energy? Dark energy is the energy needed to explain the observed accelerated expansion

More information

Decaying Dark Matter, Bulk Viscosity, and Dark Energy

Decaying Dark Matter, Bulk Viscosity, and Dark Energy Decaying Dark Matter, Bulk Viscosity, and Dark Energy Dallas, SMU; April 5, 2010 Outline Outline Standard Views Dark Matter Standard Views of Dark Energy Alternative Views of Dark Energy/Dark Matter Dark

More information

MIT Exploring Black Holes

MIT Exploring Black Holes THE UNIVERSE and Three Examples Alan Guth, MIT MIT 8.224 Exploring Black Holes EINSTEIN'S CONTRIBUTIONS March, 1916: The Foundation of the General Theory of Relativity Feb, 1917: Cosmological Considerations

More information

Gravitation: Gravitation

Gravitation: Gravitation An Introduction to General Relativity Center for Relativistic Astrophysics School of Physics Georgia Institute of Technology Notes based on textbook: Spacetime and Geometry by S.M. Carroll Spring 2013

More information

Inflation and the SLAC Theory Group I was a one-year visitor from a postdoc position at Cornell. My research problem (working with Henry Tye

Inflation and the SLAC Theory Group I was a one-year visitor from a postdoc position at Cornell. My research problem (working with Henry Tye Inflation and the SLAC Theory Group 1979 1980 I was a one-year visitor from a postdoc position at Cornell. My research problem (working with Henry Tye back at Cornell): Why were so few magnetic monopoles

More information

Inflationary Cosmology and Alternatives

Inflationary Cosmology and Alternatives Inflationary Cosmology and Alternatives V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Department of paricle Physics abd Cosmology Physics Faculty Moscow State

More information

Dark Universe II. Prof. Lynn Cominsky Dept. of Physics and Astronomy Sonoma State University

Dark Universe II. Prof. Lynn Cominsky Dept. of Physics and Astronomy Sonoma State University Dark Universe II Prof. Lynn Cominsky Dept. of Physics and Astronomy Sonoma State University Dark Universe Part II Is the universe "open" or "closed? How does dark energy change our view of the history

More information

Lecture 19. Dark Energy

Lecture 19. Dark Energy Dark Energy ΛCDM Recall the lectures on cosmology The universe is flat Total energy density is 1 We know matter and baryon density So far, we called the rest Dark Energy We treated DE in the Friedmann

More information

MODEL OF DARK MATTER AND DARK ENERGY BASED ON GRAVITATIONAL POLARIZATION. Luc Blanchet. 15 septembre 2008

MODEL OF DARK MATTER AND DARK ENERGY BASED ON GRAVITATIONAL POLARIZATION. Luc Blanchet. 15 septembre 2008 MODEL OF DARK MATTER AND DARK ENERGY BASED ON GRAVITATIONAL POLARIZATION Luc Blanchet Gravitation et Cosmologie (GRεCO) Institut d Astrophysique de Paris 15 septembre 2008 Luc Blanchet (GRεCO) Séminaire

More information

Galaxies 626. Lecture 3: From the CMBR to the first star

Galaxies 626. Lecture 3: From the CMBR to the first star Galaxies 626 Lecture 3: From the CMBR to the first star Galaxies 626 Firstly, some very brief cosmology for background and notation: Summary: Foundations of Cosmology 1. Universe is homogenous and isotropic

More information

Chapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc.

Chapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc. Chapter 23 Lecture The Cosmic Perspective Seventh Edition Dark Matter, Dark Energy, and the Fate of the Universe Curvature of the Universe The Density Parameter of the Universe Ω 0 is defined as the ratio

More information

Dark Energy and the Preposterous Universe

Dark Energy and the Preposterous Universe Dark Energy and the Preposterous Universe Sean Carroll, University of Chicago Our universe, as inventoried over the last ten years: 5% Ordinary Matter 25% Dark Matter 70% Dark Energy Dark Energy Dark Matter

More information

INFLATIONARY COSMOLOGY. and the ACCELERATING UNIVERSE. Alan Guth, MIT

INFLATIONARY COSMOLOGY. and the ACCELERATING UNIVERSE. Alan Guth, MIT INFLATIONARY COSMOLOGY and the ACCELERATING UNIVERSE Alan Guth, MIT An Open World of Physics Talks and Discussion by Friends of Fred Goldhaber Harriman Hall, SUNY Stony Brook, October 7, 2001 OUTLINE The

More information

About the format of the literature report

About the format of the literature report About the format of the literature report Minimum 3 pages! Suggested structure: Introduction Main text Discussion Conclusion References Use bracket-number (e.g. [3]) or author-year (e.g. Zackrisson et

More information

SMALL COSMOLOGICAL CONSTANT FROM RUNNING GRAVITATIONAL COUPLING

SMALL COSMOLOGICAL CONSTANT FROM RUNNING GRAVITATIONAL COUPLING SMALL COSMOLOGICAL CONSTANT FROM RUNNING GRAVITATIONAL COUPLING arxiv:1101.4995, arxiv:0803.2500 Andrei Frolov Department of Physics Simon Fraser University Jun-Qi Guo (SFU) Sternberg Astronomical Institute

More information

Cosmological Issues. Consider the stress tensor of a fluid in the local orthonormal frame where the metric is η ab

Cosmological Issues. Consider the stress tensor of a fluid in the local orthonormal frame where the metric is η ab Cosmological Issues Radiation dominated Universe Consider the stress tensor of a fluid in the local orthonormal frame where the metric is η ab ρ 0 0 0 T ab = 0 p 0 0 0 0 p 0 () 0 0 0 p We do not often

More information