Numerical Refinement of a Finite Mass Shock-Wave Cosmology
|
|
- Jack Miller
- 6 years ago
- Views:
Transcription
1 Numerical Refinement of a Finite Mass Shock-Wave Cosmology Blake Temple, UC-Davis Collaborators: J. Smoller, Z. Vogler, B. Wissman
2 References Exact solution incorporating a shock-wave into the standard FRW metric for cosmology... Smoller-Temple, Shock-Wave Cosmology Inside a Black Hole, PNAS Sept Smoller-Temple, Cosmology, Black Holes, and Shock Waves Beyond the Hubble Length, Meth. Appl. Anal., 2004.
3 References: Connecting the shock wave cosmology model with Guth s theory of inflation... How inflationary spacetimes might evolve into spacetimes of finite total mass, with J. Smoller, Meth. and Appl. of Anal., Vol. 12, No. 4, pp (2005). How inflation is used to solve the flatness problem, with J. Smoller, Jour. of Hyp. Diff. Eqns. (JHDE), Vol. 3, no. 2, (2006).
4 References: The locally inertial Glimm Scheme... A shock-wave formulation of the Einstein equations, with J. Groah, Meth. and Appl. of Anal., 7, No. 4,(2000), pp Shock-wave solutions of the Einstein equations: Existence and consistency by a locally inertial Glimm Scheme, with J. Groah, Memoirs of the AMS, Vol. 172, No. 813, November Shock Wave Interactions in General Relativity: A Locally Inertial Glimm Scheme for Spherically Symmetric Spacetimes, with J. Groah and J. Smoller, Springer Monographs in Mathematics, 2007.
5 Our Shock Wave Cosmology Solution Expanding Universe Shock Wave Matter Filled Black Hole t = 0 Big Bang t < t crit Schwarzschild Metric t = t crit Shock emerges from White Hole r = 2M = H c
6 The solution can be viewed as a natural generalization of a k=0 Oppenheimer- Snyder solution to the case of non-zero pressure, inside the Black Hole---- 2M/r>1
7 The Shock Wave Cosmology Solution Shock-Wave k=0 ds 2 = dt 2 + R(t) 2 { dr 2 + r 2 dω 2} FRW TOV: ds 2 = B( r)d t M( r) r d r 2 + r 2 dω 2 2M r > 1 r is timelike
8 1 In [Smoller-Temple, PNAS] we constructed an exact shock wave solution of the Einstein equations by matching a (k=0)- FRW metric to a TOV metric inside the Black Hole across a subluminal, entropysatisfying shock-wave, out beyond one Hubble length To obtain a large region of uniform expansion at the center consistent with observations we needed 2M r 2M > 1 r = 1 r = Hubble Length H c
9 The TOV metric inside the Black Hole is the simplest metric that cuts off the FRW at a finite total mass. Approximately like a classical explosion of finite mass with a shock-wave at the leading edge of the expansion. The solution decays time asymptotically to Oppenheimer-Snyder----a finite ball of mass expanding into empty space outside the black hole, something like a gigantic supernova.
10 Limitation of the model: TOV density and pressure are determined by the equations that describe the matching of the metrics p = c2 can only be imposed on the FRW side 3 ρ Imposing p = c2 on the TOV side introduces secondary 3 ρ waves which can not be modeled in an exact solution Question: How to model the secondary waves?
11 OUR QUESTION: How to refine the model to incorporate the correct TOV equation of state, and thereby model the secondary waves in the problem? OUR PROPOSAL: Get the initial condition at the end of inflation Use the Locally Inertial Glimm Scheme to simulate the region of interaction between the FRW and TOV metrics
12 DETAILS OF THE EXACT SOLUTION
13 The Final Equations p = σρ σ = const. Autonomous System S = 2S(1 + 3u) {(σ u) + (1 + u)s} F (S, u) u = (1 + u) { (1 3u)(σ u) + 6u(1 + u)s} G(S, u) Big Bang 0 S 1 Emerges From White Hole Entropy Condition: p < p, ρ < ρ, p < ρ S < ( ) ( ) 1 u σ u 1 + u σ + u E(u)
14 u = p ρ Entropy Inequalities 1/3 σ p < ρ p < p ρ < ρ u = E(S) S = 0 S = 1 Big Bang Solution emerges from White Hole 1 S The entropy conditions for an outgoing shock hold when u σ (S) < E(S)
15 u = p ρ Phase Portrait p = σρ 1/3 Rest Point σ < 1/3 Isocline u = E(S) σ Rest Point S = 0 Big Bang Q σ (S) u σ (S) S = 1 Solution emerges from White Hole 1 S s σ (S) shock speed < c for 0 < S < 1 s σ (S) 0 as S 0
16 u = p ρ Phase Portrait p = σρ σ = 1/3 Double Rest Point u = E(S) σ = 1/3 Isocline S = 0 Big Bang Q 1/3 (S) u σ (S) S = 1 Solution emerges from White Hole 1 S s σ (S) c as S 0
17 r = r R Shock Position= r(t) r r = c H 1 R =Hubble Length t = 0 S = 0 t = t S = 1 The Hubble length catches up to the shock-wave at S=1, the time when the entire solution emerges from the White Hole
18 Kruskall Picture 2M = 1 r t = + Black Hole Singularity FRW FRW Shock Surface FRW Universe TOV t = t Inside Black Hole Schwarzschild Spacetime Outside Black Hole p = 0 ρ = 0 p 0 ρ 0 White Hole Singularity t = 2M = 1 r
19 We are interested in the case σ = 1/3 correct for t = Big Bang to t = 10 5 yr ρ and p on the FRW and TOV side tend to the same values as t 0 It is as though the solution is emerging from a spacetime of constant density and pressure at the Big Bang Inflation
20 u = p ρ Phase Portrait p = σρ σ = 1/3 Double Rest Point u = E(S) σ = 1/3 Isocline S = 0 Big Bang Q 1/3 (S) u σ (S) S = 1 Solution emerges from White Hole 1 S s σ (S) c as S 0
21 Conclude: A solution like this would emerge at the end of inflation if the fluid at the end of inflation became co-moving wrt a (k = 0) FRW metric for r < r 0, and co-moving wrt the simplest spacetime of finite total mass for r > r 0. The inflationary disitter spacetime has all of the symmetries of a vaccuum, and so there is no preferred frame at the end of inflation
22 disitter spacetime in (k=0)-frw coordinates Finite-Mass time-slice at the end of Inflation disitter spacetime in TOV-coordinates 2M r > 1 and r timelike t = const. u co-moving wrt t = const. No preferred coordinates Inflation End of Inflation Shock T ij = ρ g ij T ij = (ρ + p)u i u j + pg ij M, r = const. u co-moving wrt M = const. (k = 0)-FRW ds 2 = dt 2 + R(t) 2 { dr 2 + r 2 dω 2} ds 2 = B( r)d t 2 + TOV 1 1 2M( r) r d r 2 + r 2 dω 2
23 time Proposed Numerical Simulation ds 2 = B( r, t)d t M( r, t) r d r 2 + r 2 dω 2 k=0 FRW metic Standard Schwarschild coordinates TOV metric inside the black hole ds 2 = dt 2 + R(t) 2 { dr 2 + r 2 dω 2} light cone ds 2 = B( r)d t M( r) r d r 2 + r 2 dω 2 space t = t 0 r = r 0 M = M( r 0 ) 2M( r 0 ) r 0 > 1 t = the end of inflation s = t 0
24 A Locally Inertial Method for Computing Shocks
25 Einstein equations-spherical Symmetry ds 2 = A(r, t)dt 2 + B(r, t)dr 2 + r 2 ( dθ 2 + sin 2 θ dφ 2) A r 2 B } {r B B + B 1 = κa 2 T 00 (1) G = 8πT 1 r 2 {r A A B t rb } = κabt 01 (2) (B 1) = κb 2 T 11 (3) 1 rab 2 {B tt A + Φ} = 2κr B T 22, (4) B = 1 1 2M r Φ = BA tb t 2AB B 2 ( Bt ) 2 A B r + AB rb + A ( ) A 2 + A A 2 A 2 A B B. (1)+(2)+(3)+(4) (1)+(3)+div T=0 (weakly)
26 References: The locally inertial Glimm Scheme... A shock-wave formulation of the Einstein equations, with J. Groah, Meth. and Appl. of Anal., 7, No. 4,(2000), pp Shock-wave solutions of the Einstein equations: Existence and consistency by a locally inertial Glimm Scheme, with J. Groah, Memoirs of the AMS, Vol. 172, No. 813, November Shock Wave Interactions in General Relativity: A Locally Inertial Glimm Scheme for Spherically Symmetric Spacetimes, with J. Groah and J. Smoller, Springer Monographs in Mathematics, 2007.
27 t Locally Inertial Glimm/Godunov Method u t + f(a, u) x = g(a, u, x) A = h(a, u, x) A 0 (t) R ij t = t j x = r 0 A ij = const. Fractional Step Method: = x i 1 u L = u i 1,j x i 1 2 R ij x i u R = u ij x i+ 1 2 x i+1 : A = A ij A = (A, B) Locally Flat in each Grid Cell Solve RP for 1/2 timestep Solve ODE for 1/2 time step Sample or Average u = (u 1, u 2 ) A = h(a, u, x) x A(r 0, t j+1 ) = A 0 (t j+1 ) p = c2 3 ρ = Nishida System = Global Exact Soln of RP, [Smol,Te]
28 Remarkable Change of Variables Equations close under change to Local Minkowski variables: I.e., Div T=0 reads: T u = T M 0 = T 00,0 + T 01, = T 01,0 + T 11, ( 2At A + B t B ) T ( At A + 3B ) t T B 2 ( 3A ( A A + B B + 4 r A + 2B B + 4 r ) ) + B t 2A T 11 T 11 + A 2B T 00 2 r B T 22 Time derivatives A t and B t cancel out under change T u Good choice because o.w. there is no A t equation to close Div T = 0! A r 2 B 1 r 2 } {r B B + B 1 {r A A = κa 2 T 00 (1) B t rb } = κabt 01 (2) (B 1) = κb 2 T 11 (3) 1 rab 2 {B tt A + Φ} = 2κr B T 22, (4)
29 Locally Inertial Formulation u = (T 00 M, T 01 M ) A = (A, B) { } { } T 00 A M +,0 B T M 01 { } { } T 01 A M +,0 B T M 11,1,1 B B A A = 2 x = 1 2 A A B = (B 1) x = (B 1) x B T 01 M, (1) { 4 x T 11 M + (B 1) (TM 00 TM 11 ) (2) x +2κxB(T 00 M T 11 M (T 01 M ) 2 ) 4xT 22}, + κxbt 00 M, (3) + κxbt 11 M. (4) TM 00 = c4 + σ 2 v 2 c 2 v 2 ρ T 01 M = c2 + σ 2 c 2 v 2 cvρ T 11 M = v2 + σ 2 c 2 v 2 ρc2 Flat Space Relativistic Euler { T 00 M },0 + { TM 10 },1 = 0 { T 01 M },0 + { TM 11 },1 = 0 u t + f(a, u) x = g(a, u, x) A = h(a, u, x)
30 Grid Rectangle R ij A = A ij u ij u i 1,j (i 12 ) (i, j (i, j) + 12 ), j Solve RP for 1 2 -timestep u t + f(a ij, u) x = 0 u = { u i 1,j u ij x x i x > x i u RP ij Solve ODE for 1 2 -timestep u t = g(a ij, u, x) A f A u(0) = u RP ij Sample/Average then update A to time t j+1 A = h(a, u, x) A(r 0, t j+1 ) = A 0 (t j+1 )
31 time Proposed Numerical Simulation ds 2 = B( r, t)d t M( r, t) r d r 2 + r 2 dω 2 k=0 FRW metic Standard Schwarschild coordinates TOV metric inside the black hole ds 2 = dt 2 + R(t) 2 { dr 2 + r 2 dω 2} light cone ds 2 = B( r)d t M( r) r d r 2 + r 2 dω 2 space t = t 0 r = r 0 M = M( r 0 ) 2M( r 0 ) r 0 > 1 t = the end of inflation s = t 0
32 Speculative Question: Could the anomolous acceleration of the Galaxies and Dark Energy be explained within Classical GR as the effect of looking out into a wave? This model represents the simplest simulation of such a wave
33 Standard Model for Dark Energy Assume Einstein equations with a cosmological constant: G ij = 8πT ij + Λg ij Assume k = 0 FRW: Leads to: ds 2 = dt 2 + R(t) 2 { dr 2 + r 2 dω 2} H 2 = κ 3 ρ + κ 3 Λ Divide by H 2 = ρ crit : 1 = Ω M + Ω Λ Best data fit leads to Ω Λ.73 and Ω M.27 Implies: The universe is 73 percent dark energy
34 Could the Anomalous acceleration be accounted for by an expansion behind the Shock Wave? Shock-Wave k=0 ds 2 = dt 2 + R(t) 2 { dr 2 + r 2 dω 2} FRW TOV: ds 2 = B( r)d t M( r) r d r 2 + r 2 dω 2 2M r > 1 r is timelike
35 Conclusion We think this numerical proposal represents a natural mathematical starting point for numerically resolving the secondary waves neglected in the exact solution. Also a possible starting point for investigating whether the anomalous acceleration/ Dark Energy could be accounted for within classical GR with classical sources?
On the occasion of the first author s seventieth birthday
METHODS AND APPLICATIONS OF ANALYSIS. c 2005 International Press Vol. 12, No. 4, pp. 451 464, December 2005 006 HOW INFLATIONARY SPACETIMES MIGHT EVOLVE INTO SPACETIMES OF FINITE TOTAL MASS JOEL SMOLLER
More informationSHOCK WAVE COSMOLOGY INSIDE A BLACK HOLE: A COMPUTER VISUALIZATION. February Abstract
SHOCK WAVE COSMOLOGY INSIDE A BLACK HOLE: A COMPUTER VISUALIZATION February 2005 JoelSmoller 1, BlakeT emple 2, ZekeV ogler 3 Abstract We discuss a computer visualization of the shock wave cosmological
More informationAn Instability of the Standard Model of Cosmology Creates the Anomalous Acceleration Without Dark Energy Revised, May 23, 2016
An Instability of the Standard Model of Cosmology Creates the Anomalous Acceleration Without Dark Energy Revised, May 23, 2016 Joel Smoller 1 Blake T emple 2 Zeke V ogler 2 Abstract: We clarify and identify
More informationHow Inflation Is Used To Resolve the Flatness Problem. September 9, To Tai-Ping Liu on the occasion of his sixtieth birthday.
How Inflation Is Used To Resolve the Flatness Problem September 9, 005 Joel Smoller Blake T emple To Tai-Ping Liu on the occasion of his sixtieth birthday. Abstract We give a mathematically rigorous exposition
More informationExpanding wave solutions of the Einstein equations that induce an anomalous acceleration into the Standard Model of Cosmology
Expanding wave solutions of the Einstein equations that induce an anomalous acceleration into the Standard odel of Cosmology Blake Temple a,,2 and Joel Smoller b,,2 a Department of athematics, University
More informationA SHOCK WAVE REFINEMENT of the FRIEDMANN-ROBERTSON-WALKER METRIC November 28, 2003
A SHOCK WAVE REFINEMENT of the FRIEDMANN-ROBERTSON-WALKER METRIC November 28, 2003 Joel Smoller 1 Blake T emple 2 1 Introduction In the standard model of cosmology, the expanding universe of galaxies is
More informationKerr black hole and rotating wormhole
Kerr Fest (Christchurch, August 26-28, 2004) Kerr black hole and rotating wormhole Sung-Won Kim(Ewha Womans Univ.) August 27, 2004 INTRODUCTION STATIC WORMHOLE ROTATING WORMHOLE KERR METRIC SUMMARY AND
More informationc 2001 International Press Vol. 8, No. 4, pp , December
METHODS AND APPLICATIONS OF ANALYSIS. c 2001 International Press Vol. 8, No. 4, pp. 599 608, December 2001 010 THEORY OF A COSMIC SHOCK-WAVE JOEL SMOLLER AND BLAKE TEMPLE Abstract. We discuss mathematical
More informationGeneral Relativity and Cosmology. The End of Absolute Space Cosmological Principle Black Holes CBMR and Big Bang
General Relativity and Cosmology The End of Absolute Space Cosmological Principle Black Holes CBMR and Big Bang The End of Absolute Space (AS) Special Relativity (SR) abolished AS only for the special
More informationCosmology with a Shock-Wave
Commun. Math. Phys. 210, 275 308 (2000) Communications in Mathematical Physics Springer-Verlag 2000 Cosmology with a Shock-Wave Joel Smoller 1,, Blake Temple 2, 1 Department of Mathematics, University
More informationPHYM432 Relativity and Cosmology 17. Cosmology Robertson Walker Metric
PHYM432 Relativity and Cosmology 17. Cosmology Robertson Walker Metric Cosmology applies physics to the universe as a whole, describing it s origin, nature evolution and ultimate fate. While these questions
More informationPROBLEM SET 10 (The Last!)
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Physics 8.286: The Early Universe December 8, 2016 Prof. Alan Guth PROBLEM SET 10 (The Last!) DUE DATE: Wednesday, December 14, 2016, at 4:00 pm.
More information12. Relativistic Cosmology I. Simple Solutions to the Einstein Equations
12. Relativistic Cosmology I. Simple Solutions to the Einstein Equations 1. Minkowski space Initial assumptions:! no matter (T µν = 0)! no gravitation (R σ µνρ = 0; i.e., zero curvature) Not realistic!
More informationKinetic Theory of Dark Energy within General Relativity
Kinetic Theory of Dark Energy within General Relativity Author: Nikola Perkovic* percestyler@gmail.com University of Novi Sad, Faculty of Sciences, Institute of Physics and Mathematics Abstract: This paper
More informationCurved Spacetime III Einstein's field equations
Curved Spacetime III Einstein's field equations Dr. Naylor Note that in this lecture we will work in SI units: namely c 1 Last Week s class: Curved spacetime II Riemann curvature tensor: This is a tensor
More informationQuantum Gravity and Black Holes
Quantum Gravity and Black Holes Viqar Husain March 30, 2007 Outline Classical setting Quantum theory Gravitational collapse in quantum gravity Summary/Outlook Role of metrics In conventional theories the
More informationÜbungen zu RT2 SS (4) Show that (any) contraction of a (p, q) - tensor results in a (p 1, q 1) - tensor.
Übungen zu RT2 SS 2010 (1) Show that the tensor field g µν (x) = η µν is invariant under Poincaré transformations, i.e. x µ x µ = L µ νx ν + c µ, where L µ ν is a constant matrix subject to L µ ρl ν ση
More information2.1 Basics of the Relativistic Cosmology: Global Geometry and the Dynamics of the Universe Part I
1 2.1 Basics of the Relativistic Cosmology: Global Geometry and the Dynamics of the Universe Part I 2 Special Relativity (1905) A fundamental change in viewing the physical space and time, now unified
More information3.1 Cosmological Parameters
3.1 Cosmological Parameters 1 Cosmological Parameters Cosmological models are typically defined through several handy key parameters: Hubble Constant Defines the Scale of the Universe R 0 H 0 = slope at
More informationCosmology 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 informationCosmology and particle physics
Cosmology and particle physics Lecture notes Timm Wrase Lecture 9 Inflation - part I Having discussed the thermal history of our universe and in particular its evolution at times larger than 10 14 seconds
More informationCausal nature and dynamics of trapping horizon in black hole collapse
Causal nature and dynamics of trapping horizon in black hole collapse Ilia Musco (CNRS, Observatoire de Paris/Meudon - LUTH) KSM 2017- FIAS (Frankfurt) 24-28 July 2017 Classical and Quantum Gravity Vol.
More informationPROBLEM SET 6 EXTRA CREDIT PROBLEM SET
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Physics 8.286: The Early Universe May 3, 2004 Prof. Alan Guth PROBLEM SET 6 EXTRA CREDIT PROBLEM SET CAN BE HANDED IN THROUGH: Thursday, May 13,
More informationNew 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 informationCosmological Confusion
Cosmological Confusion revealing common misconceptions about the big bang, the expansion of the universe and cosmic horizons. Cosmological confusion Dark energy the first confusion. coordinates and velocities
More informationRelativity, 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 informationLecture 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 informationCosmology (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 informationFrom An Apple To Black Holes Gravity in General Relativity
From An Apple To Black Holes Gravity in General Relativity Gravity as Geometry Central Idea of General Relativity Gravitational field vs magnetic field Uniqueness of trajectory in space and time Uniqueness
More informationThe Apparent Universe
The Apparent Universe Alexis HELOU APC - AstroParticule et Cosmologie, Paris, France alexis.helou@apc.univ-paris7.fr 11 th June 2014 Reference This presentation is based on a work by P. Binétruy & A. Helou:
More informationMASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Physics 8.286: The Early Universe October 27, 2013 Prof. Alan Guth PROBLEM SET 6
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Physics 8.86: The Early Universe October 7, 013 Prof. Alan Guth PROBLEM SET 6 DUE DATE: Monday, November 4, 013 READING ASSIGNMENT: Steven Weinberg,
More informationLecture 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 informationAnalytic Kerr Solution for Puncture Evolution
Analytic Kerr Solution for Puncture Evolution Jon Allen Maximal slicing of a spacetime with a single Kerr black hole is analyzed. It is shown that for all spin parameters, a limiting hypersurface forms
More informationPhysics 325: General Relativity Spring Final Review Problem Set
Physics 325: General Relativity Spring 2012 Final Review Problem Set Date: Friday 4 May 2012 Instructions: This is the third of three review problem sets in Physics 325. It will count for twice as much
More informationCosmological 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 informationGeneral Birkhoff s Theorem
General Birkhoff s Theorem Amir H. Abbassi Department of Physics, School of Sciences, Tarbiat Modarres University, P.O.Box 14155-4838, Tehran, I.R.Iran E-mail: ahabbasi@net1cs.modares.ac.ir Abstract Space-time
More informationDecaying 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 informationGeneral Relativity and Cosmology Mock exam
Physikalisches Institut Mock Exam Universität Bonn 29. June 2011 Theoretische Physik SS 2011 General Relativity and Cosmology Mock exam Priv. Doz. Dr. S. Förste Exercise 1: Overview Give short answers
More information1. De Sitter Space. (b) Show that the line element for a positively curved FRW model (k = +1) with only vacuum energy (P = ) is
1. De Sitter Space (a) Show in the context of expanding FRW models that if the combination +3P is always positive, then there was a Big Bang singularity in the past. [A sketch of a(t) vs.t may be helpful.]
More informationSOLVING THE HORIZON PROBLEM WITH A DELAYED BIG-BANG SINGULARITY
SOLVING THE HORIZON PROBLEM WITH A DELAYED BIG-BANG SINGULARITY Marie-Noëlle CÉLÉRIER Département d Astrophysique Relativiste et de Cosmologie Observatoire de Paris Meudon 5 Place Jules Janssen 92195 Meudon
More informationDynamical compactification from higher dimensional de Sitter space
Dynamical compactification from higher dimensional de Sitter space Matthew C. Johnson Caltech In collaboration with: Sean Carroll Lisa Randall 0904.3115 Landscapes and extra dimensions Extra dimensions
More informationThe Geometry of Relativity
The Geometry of Relativity Tevian Dray Department of Mathematics Oregon State University http://www.math.oregonstate.edu/~tevian PNWMAA 4/11/15 Tevian Dray The Geometry of Relativity 1/25 Books The Geometry
More informationLecture Notes on General Relativity
Lecture Notes on General Relativity Matthias Blau Albert Einstein Center for Fundamental Physics Institut für Theoretische Physik Universität Bern CH-3012 Bern, Switzerland The latest version of these
More informationOddities of the Universe
Oddities of the Universe Koushik Dutta Theory Division, Saha Institute Physics Department, IISER, Kolkata 4th November, 2016 1 Outline - Basics of General Relativity - Expanding FRW Universe - Problems
More informationWHY BLACK HOLES PHYSICS?
WHY BLACK HOLES PHYSICS? Nicolò Petri 13/10/2015 Nicolò Petri 13/10/2015 1 / 13 General motivations I Find a microscopic description of gravity, compatibile with the Standard Model (SM) and whose low-energy
More informationExact Solutions of the Einstein Equations
Notes from phz 6607, Special and General Relativity University of Florida, Fall 2004, Detweiler Exact Solutions of the Einstein Equations These notes are not a substitute in any manner for class lectures.
More informationThe cosmic horizon. Fulvio Melia Department of Physics and Steward Observatory, The University of Arizona, Tucson, Arizona 85721, USA
Mon. Not. R. Astron. Soc. 382, 1917 1921 (2007) doi:10.1111/j.1365-2966.2007.12499.x The cosmic horizon Fulvio Melia Department of Physics and Steward Observatory, The University of Arizona, Tucson, Arizona
More informationAccelerating Cosmologies and Black Holes in the Dilatonic Einstein-Gauss-Bonnet (EGB) Theory
Accelerating Cosmologies and Black Holes in the Dilatonic Einstein-Gauss-Bonnet (EGB) Theory Zong-Kuan Guo Fakultät für Physik, Universität Bielefeld Zong-Kuan Guo (Universität Bielefeld) Dilatonic Einstein-Gauss-Bonnet
More informationLecture 14: Cosmological Principles
Lecture 14: Cosmological Principles The basic Cosmological Principles The geometry of the Universe The scale factor R and curvature constant k Comoving coordinates Einstein s initial solutions 3/28/11
More informationGravitation: Cosmology
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 informationThe Geometry of Relativity
The Geometry of Relativity Tevian Dray Department of Mathematics Oregon State University http://www.math.oregonstate.edu/~tevian OSU 4/27/15 Tevian Dray The Geometry of Relativity 1/27 Books The Geometry
More informationNon Linear Dynamics in Einstein-Friedman Equations
Non Linear Dynamics in Einstein-Friedman Equations Usman Naseer 2012-10-0054 May 15, 2011 Abstract Einstein-Friedman equations for the dynamics of a spatially homogenous and isotropic universe are rederived
More informationHOMEWORK 10. Applications: special relativity, Newtonian limit, gravitational waves, gravitational lensing, cosmology, 1 black holes
General Relativity 8.96 (Petters, spring 003) HOMEWORK 10. Applications: special relativity, Newtonian limit, gravitational waves, gravitational lensing, cosmology, 1 black holes 1. Special Relativity
More informationGeneral 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 informationA A + B. ra + A + 1. We now want to solve the Einstein equations in the following cases:
Lecture 29: Cosmology Cosmology Reading: Weinberg, Ch A metric tensor appropriate to infalling matter In general (see, eg, Weinberg, Ch ) we may write a spherically symmetric, time-dependent metric in
More informationComputational Physics and Astrophysics
Cosmological Inflation Kostas Kokkotas University of Tübingen, Germany and Pablo Laguna Georgia Institute of Technology, USA Spring 2012 Our Universe Cosmic Expansion Co-moving coordinates expand at exactly
More informationA Hypothesis Connecting Dark Energy, Virtual Gravitons, and the Holographic Entropy Bound. Claia Bryja City College of San Francisco
A Hypothesis Connecting Dark Energy, Virtual Gravitons, and the Holographic Entropy Bound Claia Bryja City College of San Francisco The Holographic Principle Idea proposed by t Hooft and Susskind (mid-
More informationA Curvature Primer. With Applications to Cosmology. Physics , General Relativity
With Applications to Cosmology Michael Dine Department of Physics University of California, Santa Cruz November/December, 2009 We have barely three lectures to cover about five chapters in your text. To
More informationKinematics of time within General Relativity
Kinematics of time within General Relativity by Nikola Perkovic e-mail: perce90gm@gmail.com Institute of Physics and Mathematics, Faculty of Sciences, University of Novi Sad Abstract: This paper will provide
More informationA5682: Introduction to Cosmology Course Notes. 2. General Relativity
2. General Relativity Reading: Chapter 3 (sections 3.1 and 3.2) Special Relativity Postulates of theory: 1. There is no state of absolute rest. 2. The speed of light in vacuum is constant, independent
More informationBlack-Hole Solutions with Scalar Hair in Einstein-Scalar-Gauss-Bonnet Theories
Black-Hole Solutions with Scalar Hair in Einstein-Scalar-Gauss-Bonnet Theories Athanasios Bakopoulos Physics Department University of Ioannina In collaboration with: George Antoniou and Panagiota Kanti
More informationLaw of Gravity, Dark Matter and Dark Energy
Law of Gravity, Dark Matter and Dark Energy Tian Ma, Shouhong Wang Supported in part by NSF, ONR and Chinese NSF Blog: http://www.indiana.edu/~fluid https://physicalprinciples.wordpress.com I. Laws of
More informationEinstein Double Field Equations
Einstein Double Field Equations Stephen Angus Ewha Woman s University based on arxiv:1804.00964 in collaboration with Kyoungho Cho and Jeong-Hyuck Park (Sogang Univ.) KIAS Workshop on Fields, Strings and
More informationPhysics 311 General Relativity. Lecture 18: Black holes. The Universe.
Physics 311 General Relativity Lecture 18: Black holes. The Universe. Today s lecture: Schwarzschild metric: discontinuity and singularity Discontinuity: the event horizon Singularity: where all matter
More informationTheory. V H Satheeshkumar. XXVII Texas Symposium, Dallas, TX December 8 13, 2013
Department of Physics Baylor University Waco, TX 76798-7316, based on my paper with J Greenwald, J Lenells and A Wang Phys. Rev. D 88 (2013) 024044 with XXVII Texas Symposium, Dallas, TX December 8 13,
More informationGeneral Relativity ASTR 2110 Sarazin. Einstein s Equation
General Relativity ASTR 2110 Sarazin Einstein s Equation Curvature of Spacetime 1. Principle of Equvalence: gravity acceleration locally 2. Acceleration curved path in spacetime In gravitational field,
More informationAn Overview of Mathematical General Relativity
An Overview of Mathematical General Relativity José Natário (Instituto Superior Técnico) Geometria em Lisboa, 8 March 2005 Outline Lorentzian manifolds Einstein s equation The Schwarzschild solution Initial
More informationEinstein s Theory of Gravity. December 13, 2017
December 13, 2017 Newtonian Gravity Poisson equation 2 U( x) = 4πGρ( x) U( x) = G ρ( x) x x d 3 x For a spherically symmetric mass distribution of radius R U(r) = 1 r U(r) = 1 r R 0 r 0 r 2 ρ(r )dr for
More informationThe Stability of the Irrotational Euler-Einstein System with a Positive Cosmological Constant
The Stability of the Irrotational Euler-Einstein System with a Positive Cosmological Constant Jared Speck & Igor Rodnianski jspeck@math.princeton.edu University of Cambridge & Princeton University October
More informationIntroduction to Cosmology
Introduction to Cosmology João G. Rosa joao.rosa@ua.pt http://gravitation.web.ua.pt/cosmo LECTURE 2 - Newtonian cosmology I As a first approach to the Hot Big Bang model, in this lecture we will consider
More informationDerivation of relativistic Burgers equation on de Sitter background
Derivation of relativistic Burgers equation on de Sitter background BAVER OKUTMUSTUR Middle East Technical University Department of Mathematics 06800 Ankara TURKEY baver@metu.edu.tr TUBA CEYLAN Middle
More informationAstr 2320 Tues. May 2, 2017 Today s Topics Chapter 23: Cosmology: The Big Bang and Beyond Introduction Newtonian Cosmology Solutions to Einstein s
Astr 0 Tues. May, 07 Today s Topics Chapter : Cosmology: The Big Bang and Beyond Introduction Newtonian Cosmology Solutions to Einstein s Field Equations The Primeval Fireball Standard Big Bang Model Chapter
More informationPOINTS OF GENERAL RELATIVISITIC SHOCK WAVE INTERACTION ARE REGULARITY SINGULARITIES WHERE SPACETIME IS NOT LOCALLY FLAT
POINTS OF GENERAL RELATIVISITIC SHOCK WAVE INTERACTION ARE REGULARITY SINGULARITIES WHERE SPACETIME IS NOT LOCALLY FLAT MORITZ REINTJES AND BLAKE TEMPLE APRIL 2011 Abstract. We show that the regularity
More informationEinstein s Equations. July 1, 2008
July 1, 2008 Newtonian Gravity I Poisson equation 2 U( x) = 4πGρ( x) U( x) = G d 3 x ρ( x) x x For a spherically symmetric mass distribution of radius R U(r) = 1 r U(r) = 1 r R 0 r 0 r 2 ρ(r )dr for r
More informationSCIENTIFIC UNDERSTANDING OF THE ANISOTROPIC UNIVERSE IN THE WARPED PRODUCTS SPACETIME FOR AEROSPACE POWER. Jaedong Choi
Korean J. Math. 23 (2015) No. 3 pp. 479 489 http://dx.doi.org/10.11568/kjm.2015.23.3.479 SCIENTIFIC UNDERSTANDING OF THE ANISOTROPIC UNIVERSE IN THE WARPED PRODUCTS SPACETIME FOR AEROSPACE POWER Jaedong
More information8 Cosmology. December 1997 Lecture Notes on General Relativity Sean M. Carroll
December 1997 Lecture Notes on General Relativity Sean M. Carroll 8 Cosmology Contemporary cosmological models are based on the idea that the universe is pretty much the same everywhere a stance sometimes
More informationRelativity SPECIAL, GENERAL, AND COSMOLOGICAL SECOND EDITION. Wolfgang Rindler. Professor of Physics The University of Texas at Dallas
Relativity SPECIAL, GENERAL, AND COSMOLOGICAL SECOND EDITION Wolfgang Rindler Professor of Physics The University of Texas at Dallas OXPORD UNIVERSITY PRESS Contents Introduction l 1 From absolute space
More informationDark 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 informationBachelor Thesis. General Relativity: An alternative derivation of the Kruskal-Schwarzschild solution
Bachelor Thesis General Relativity: An alternative derivation of the Kruskal-Schwarzschild solution Author: Samo Jordan Supervisor: Prof. Markus Heusler Institute of Theoretical Physics, University of
More informationGeneral relativity and the Einstein equations
April 23, 2013 Special relativity 1905 Let S and S be two observers moving with velocity v relative to each other along the x-axis and let (t, x) and (t, x ) be the coordinate systems used by these observers.
More informationConserved Quantities in Lemaître-Tolman-Bondi Cosmology
1/15 Section 1 Section 2 Section 3 Conserved Quantities in Lemaître-Tolman-Bondi Cosmology Alex Leithes - Blackboard Talk Outline ζ SMTP Evolution Equation: ζ SMTP = H X + 2H Y 3 ρ Valid on all scales.
More informationCosmology: The Origin and Evolution of the Universe Chapter Twenty-Eight. Guiding Questions
Cosmology: The Origin and Evolution of the Universe Chapter Twenty-Eight Guiding Questions 1. What does the darkness of the night sky tell us about the nature of the universe? 2. As the universe expands,
More informationFinite volume approximation of the relativistic Burgers equation on a Schwarzschild (anti-)de Sitter spacetime
Turkish Journal of Mathematics http:// journals. tubitak. gov. tr/ math/ Research Article Turk J Math 2017 41: 1027 1041 c TÜBİTAK doi:10.906/mat-1602-8 Finite volume approximation of the relativistic
More informationChapter 12. Quantum black holes
Chapter 12 Quantum black holes Classically, the fundamental structure of curved spacetime ensures that nothing can escape from within the Schwarzschild event horizon. That is an emphatically deterministic
More informationPAPER 71 COSMOLOGY. Attempt THREE questions There are seven questions in total The questions carry equal weight
MATHEMATICAL TRIPOS Part III Friday 31 May 00 9 to 1 PAPER 71 COSMOLOGY Attempt THREE questions There are seven questions in total The questions carry equal weight You may make free use of the information
More informationGeneral Relativity and Differential
Lecture Series on... General Relativity and Differential Geometry CHAD A. MIDDLETON Department of Physics Rhodes College November 1, 2005 OUTLINE Distance in 3D Euclidean Space Distance in 4D Minkowski
More informationSet 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 informationArvind 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 informationTHE 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 informationWhy is the Universe Expanding?
Why is the Universe Expanding? In general relativity, mass warps space. Warped space makes matter move, which changes the structure of space. Thus the universe should be dynamic! Gravity tries to collapse
More information8.821/8.871 Holographic duality
Lecture 3 8.81/8.871 Holographic duality Fall 014 8.81/8.871 Holographic duality MIT OpenCourseWare Lecture Notes Hong Liu, Fall 014 Lecture 3 Rindler spacetime and causal structure To understand the spacetime
More informationIntroduction 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 informationModeling the Universe A Summary
Modeling the Universe A Summary Questions to Consider 1. What does the darkness of the night sky tell us about the nature of the universe? 2. As the universe expands, what, if anything, is it expanding
More informationcarroll/notes/ has a lot of good notes on GR and links to other pages. General Relativity Philosophy of general
http://pancake.uchicago.edu/ carroll/notes/ has a lot of good notes on GR and links to other pages. General Relativity Philosophy of general relativity. As with any major theory in physics, GR has been
More informationThe Influence of DE on the Expansion Rate of the Universe and its Effects on DM Relic Abundance
The Influence of DE on the Expansion Rate of the Universe and its Effects on DM Relic Abundance Esteban Jimenez Texas A&M University XI International Conference on Interconnections Between Particle Physics
More informationGravitational collapse and the vacuum energy
Journal of Physics: Conference Series OPEN ACCESS Gravitational collapse and the vacuum energy To cite this article: M Campos 2014 J. Phys.: Conf. Ser. 496 012021 View the article online for updates and
More informationA glimpse on Cosmology: Mathematics meets the Data
Naples 09 Seminar A glimpse on Cosmology: Mathematics meets the Data by 10 November 2009 Monica Capone 1 Toward a unified epistemology of Sciences...As we know, There are known knowns. There are things
More information14. Black Holes 2 1. Conformal Diagrams of Black Holes
14. Black Holes 2 1. Conformal Diagrams of Black Holes from t = of outside observer's clock to t = of outside observer's clock time always up light signals always at 45 time time What is the causal structure
More informationCalculating Accurate Waveforms for LIGO and LISA Data Analysis
Calculating Accurate Waveforms for LIGO and LISA Data Analysis Lee Lindblom Theoretical Astrophysics, Caltech HEPL-KIPAC Seminar, Stanford 17 November 2009 Results from the Caltech/Cornell Numerical Relativity
More informationWeek 2 Part 2. The Friedmann Models: What are the constituents of the Universe?
Week Part The Friedmann Models: What are the constituents of the Universe? We now need to look at the expansion of the Universe described by R(τ) and its derivatives, and their relation to curvature. For
More information