Inflation, Tuning and Measures
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1 Inflation, Tuning and Measures Andreas Albrecht; UC Davis Cosmocruise Sep Albrecht CosmoCruise 9/5/15 1
2 Inflation, Tuning and Measures THANKS! Andreas Albrecht; UC Davis Cosmocruise Sep Albrecht CosmoCruise 9/5/15 2
3 Inflation, Tuning and Measures THANKS! Andreas Albrecht; UC Davis Cosmocruise Sep Albrecht CosmoCruise 9/5/15 3
4 Inflation, Tuning and Measures A complement to Alexei s talk Andreas Albrecht; UC Davis Cosmocruise Sep Albrecht CosmoCruise 9/5/15 4
5 The History of the Universe Albrecht CosmoCruise 9/5/15 5
6 The History of the Universe NO Albrecht CosmoCruise 9/5/15 6
7 The History of the Universe? Albrecht CosmoCruise 9/5/15 7
8 Planck Data Albrecht CosmoCruise 9/5/15 8
9 Planck Data Cosmic Inflation theory Albrecht CosmoCruise 9/5/15 9
10 Planck Data Cosmic Inflation theory Albrecht CosmoCruise 9/5/15 10
11 Planck Data Cosmic Inflation theory Albrecht CosmoCruise 9/5/15 11
12 A recent application of inflation (IAU 2015) Albrecht CosmoCruise 9/5/15 12
13 Cosmic Inflation: Great phenomenology of cosmic structure, but: Albrecht CosmoCruise 9/5/15 13
14 Cosmic Inflation: Great phenomenology of cosmic structure, but: Albrecht CosmoCruise 9/5/15 14
15 Cosmic Inflation: Great phenomenology of cosmic structure, but: 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) Albrecht CosmoCruise 9/5/15 15
16 Cosmic Inflation: Great phenomenology of cosmic structure, but: 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) 2) Concreteness: Measure problems etc. Albrecht CosmoCruise 9/5/15 16
17 Cosmic Inflation: Great phenomenology of cosmic structure, but: This Talk 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) 2) Concreteness: Measure problems etc. Albrecht CosmoCruise 9/5/15 17
18 Cosmic Inflation: Great phenomenology of cosmic structure, but: This Talk 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) 2) Concreteness: Measure problems etc. But should we care? Albrecht CosmoCruise 9/5/15 18
19 Cosmic Inflation: Great phenomenology of cosmic structure, but: This Talk 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) 2) Concreteness: Measure problems etc. vs normal physics theory (e.g. Starobinsky s talk) But should we care? Albrecht CosmoCruise 9/5/15 19
20 Cosmic Inflation: Great phenomenology of cosmic structure, but: This Talk 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) 2) Concreteness: Measure problems etc. vs normal physics theory (e.g. Starobinsky s talk) But should we care? Is it the right time to explore these questions? Albrecht CosmoCruise 9/5/15 20
21 Cosmic Inflation: Great phenomenology of cosmic structure, but: 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) Should we just be happy with this? 2) Concreteness: Measure problems etc. vs normal physics theory (e.g. Starobinsky s talk) But should we care? Is it the right time to explore these questions Albrecht CosmoCruise 9/5/15 21
22 Cosmic Inflation: Unresolved mysteries Great phenomenology of cosmic structure, but: 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) Should we just be happy with this? 2) Concreteness: Measure problems etc. vs normal physics theory (e.g. Starobinsky s talk) But should we care? Is it the right time to explore these questions Albrecht CosmoCruise 9/5/15 22
23 Cosmic Inflation: Consumers & Producers Albrecht CosmoCruise 9/5/15 23
24 Cosmic Inflation: Consumers & Producers Albrecht CosmoCruise 9/5/15 24
25 Goal of resolving tuning inspired by Guth s paper: Albrecht CosmoCruise 9/5/15 25
26 An alternate perspective in Starobinsky s famous paper: Albrecht CosmoCruise 9/5/15 26
27 Cosmic Inflation: Unresolved mysteries Great phenomenology of cosmic structure, but: 1) Tuning: Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. (We have not succeeded so far.) Should we just be happy with this? 2) Concreteness: Measure problems etc. vs normal physics theory (e.g. Starobinsky s talk) But should we care? Is it the right time to explore these questions Albrecht CosmoCruise 9/5/15 27
28 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 28
29 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 29
30 What is tuning? Albrecht CosmoCruise 9/5/15 30
31 What is tuning? You are here Phase Space Albrecht CosmoCruise 9/5/15 31
32 What is tuning? You are here Pencil Analogy Phase Space Albrecht CosmoCruise 9/5/15 32
33 What is tuning? You are here Pencil Analogy Phase vsspace Albrecht CosmoCruise 9/5/15 33
34 What is tuning? You are here Phase Space Albrecht CosmoCruise 9/5/15 34
35 What is tuning? You are here Box of gas anaogy Phase Space vs Albrecht CosmoCruise 9/5/15 35
36 In the SBB, flatness & homogeneity are unstable fixed points : c c 2 3H 8 1 a 2 a 2 8 a H 3 k a 2 At or T a a GeV The GUT scale a 3, a 4 Dominates with time Require c to 55 decimal places to get Albrecht CosmoCruise 9/5/15 c today 36
37 What is tuning? You are here Phase Space Albrecht CosmoCruise 9/5/15 37
38 What is the 2 nd law? Albrecht CosmoCruise 9/5/15 38
39 What is the 2 nd law? S ln N You are here Phase Space Albrecht CosmoCruise 9/5/15 39
40 What is the 2 nd law? S ln N You are here 2 nd law tuning? Phase Space Albrecht CosmoCruise 9/5/15 40
41 What is the 2 nd law? S ln N You are here 2 nd law tuning? Phase Space Is the only way to avoid tuning to abandon the 2 nd law? Albrecht CosmoCruise 9/5/15 41
42 S Today Albrecht CosmoCruise 9/5/15 42 t
43 S Statistical arguments Today Albrecht CosmoCruise 9/5/15 43 t
44 S Statistical arguments Today Albrecht CosmoCruise 9/5/15 44 t
45 S Statistical arguments What we actually believe Today Albrecht CosmoCruise 9/5/15 45 t
46 S Statistical arguments What we actually believe Today The thermodynamic arrow of time The past hypothesis = Fine tuning Albrecht CosmoCruise 9/5/15 46 t
47 S Statistical arguments What we actually believe Adding reheating and inflation seems to make all this worse Today The thermodynamic arrow of time The past hypothesis = Fine tuning Albrecht CosmoCruise 9/5/15 47 t
48 S Statistical arguments What we actually believe Adding reheating and inflation seems to make all this worse Today The thermodynamic arrow of time The past hypothesis = Fine tuning Albrecht CosmoCruise 9/5/15 48 t
49 S Statistical arguments What we actually believe Adding reheating and inflation seems to make all this worse Low entropy of early universe Today (SBB) = low *gravitational* entropy The = FRW thermodynamic (Penrose) arrow of time The past hypothesis = Fine tuning Albrecht CosmoCruise 9/5/15 49 t
50 S Statistical arguments What we actually believe Adding reheating and inflation seems to make all this worse Low entropy of early universe Today (SBB) = low *gravitational* entropy The = FRW thermodynamic (Penrose) arrow of time Related to Starobinsky comment about finding a black hole The past hypothesis = Fine tuning Albrecht CosmoCruise 9/5/15 50 t
51 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 51
52 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 52
53 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Albrecht CosmoCruise 9/5/15 53
54 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: Albrecht CosmoCruise 9/5/15 54
55 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: String Theory Landscape (Arrival Terminals) Albrecht CosmoCruise 9/5/15 55
56 Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Stoltenberg & AA 2015 Related issues: String Theory Landscape (Arrival Terminals) Albrecht CosmoCruise 9/5/15 56
57 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: String Theory Landscape (Arrival Terminals) Tuning assumptions in infinite universes (eternal) Albrecht CosmoCruise 9/5/15 57
58 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: String Theory Landscape (Arrival Terminals) Tuning assumptions in infinite universes (eternal) Hernley, AA & Dray 2013 Albrecht CosmoCruise 9/5/15 58
59 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: String Theory Landscape (Arrival Terminals) Tuning assumptions in infinite universes (eternal) Various discussions about tuning in SBB (with or without inflation) Albrecht CosmoCruise 9/5/15 59
60 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: String Theory Landscape (Arrival Terminals) Tuning assumptions in infinite universes (eternal) Various discussions about tuning in SBB (with or without inflation) Gibbons & Turok Dyson et al. Carroll & Tam Shiffren & Wald Penrose Albrecht CosmoCruise 9/5/15 60
61 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: String Theory Landscape (Arrival Terminals) Tuning assumptions in infinite universes (eternal) Various discussions about tuning in SBB (with or without inflation) Gibbons & Turok Dyson et al Carroll & Tam Shiffren & Wald Penrose NB Same issues with cyclic models: S 0 but it s infinite (!) Albrecht CosmoCruise 9/5/15 61
62 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: String Theory Landscape (Arrival Terminals) Tuning assumptions in infinite universes (eternal) Various discussions about tuning in SBB (with or without inflation) Gibbons & Turok Dyson et al. Carroll & Tam Shiffren & Wald Penrose NB Same issues with cyclic models: S 0 but it s infinite (!) Albrecht CosmoCruise 9/5/15 62
63 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: Arrival Terminals Tuning assumptions in infinite universes (eternal) Various discussions about tuning in SBB (with or without inflation) Belief in naturalness of high energy density starts Std inflation Landscape Albrecht CosmoCruise 9/5/15 63
64 Beware temporal provincialism : 3 Equipartition argument (equally likely anywhere on potential) 4 V/M Plank /M P ϕ/m Plank Albrecht CosmoCruise 9/5/15 64
65 4 V/M Plank Beware temporal provincialism : Equipartition argument (equally likely anywhere on potential) /M ϕ/m Plank P Albrecht CosmoCruise 9/5/15 65
66 Beware temporal provincialism : 3 Equipartition argument (equally likely anywhere on potential) 4 V/M Plank 2 1 Entropy arguments give exponential 0 M exp 2 /M ϕ/m V V values 2 Plank P suppression of higher P 12 exp exp exp exp S Albrecht CosmoCruise 9/5/15 66 S S 1 1 S 1 2 M V M V 4 4 P P 1 2
67 Beware temporal provincialism : 3 Equipartition argument (equally likely anywhere on potential) 4 V/M Plank 2 Why would you want to start with high entropy? You 1should end with that Entropy arguments give exponential 0 M exp 2 /M ϕ/m V V values 2 Plank P suppression of higher P 12 exp exp exp exp S Albrecht CosmoCruise 9/5/15 67 S S 1 1 S 1 2 M V M V 4 4 P P 1 2
68 Beware temporal provincialism : 3 Equipartition argument (equally likely anywhere on potential) 4 V/M Plank 2 Why would you want to start with high entropy? You 1should end with that Entropy arguments give exponential 0 M exp 2 /M ϕ/m V V values 2 Plank P suppression of higher P 12 exp exp exp exp S Albrecht CosmoCruise 9/5/15 68 S S 1 1 S 1 2 M V M V 4 4 P P 1 2
69 Beware temporal provincialism : Beware temporal provincialism : The tendency to slip in assumptions about (and thus tunings of initial conditions) without even realizing it S 0 Related issues: Arrival Terminals Tuning assumptions in infinite universes (eternal) Various discussions about tuning in SBB (with or without inflation) Belief in naturalness of high energy density starts Albrecht CosmoCruise 9/5/15 69
70 But if eternal inflation produces an infinite universe surely it does not matter if the start of inflation is very improbable Albrecht CosmoCruise 9/5/15 70
71 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 71
72 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 72
73 Slow rolling of inflaton 2.5 x V/M GUT Observable physics generated here /M P Albrecht CosmoCruise 9/5/15 73
74 Slow rolling of inflaton 2.5 x V/M GUT Observable physics generated here Extrapolating back /M P Albrecht CosmoCruise 9/5/15 74
75 2.5 x Slow rolling of inflaton Self reproducing regime (dominated by quantum fluctuations): Eternal inflation/multiverse Q 4 V/M GUT Observable physics generated here Extrapolating back /M P Albrecht CosmoCruise 9/5/15 75
76 2.5 x Slow rolling of inflaton Self reproducing regime (dominated by quantum fluctuations): Eternal inflation/multiverse Q 4 V/M GUT Observable physics generated here Extrapolating back /M P Albrecht CosmoCruise 9/5/15 76
77 The multiverse of eternal inflation Self reproduction regime Classically Rolling Classically Rolling Albrecht CosmoCruise 9/5/15 77
78 The multiverse of eternal inflation Self reproduction regime Classically Rolling Where are we? (Young universe, old universe, curvature etc) Classically Rolling Albrecht CosmoCruise 9/5/15 78
79 The multiverse of eternal inflation with multiple classical rolling directions Self reproduction regime Classically Rolling A Classically Rolling B Classically Rolling C Classically Rolling D Albrecht CosmoCruise 9/5/15 79
80 The multiverse of eternal inflation with multiple classical rolling directions Self reproduction regime Classically Rolling A Classically Rolling B Where are we? (Young universe, old universe, curvature, physical properties A, B, C, D, etc) Classically Rolling C Classically Rolling D Albrecht CosmoCruise 9/5/15 80
81 The multiverse of eternal inflation with multiple classical rolling directions Self reproduction regime Classically Rolling A Classically Rolling B Where Classically are we? Rolling Where are we? (Young universe, old universe, Expect the C theory to curvature, physical properties A, B, C, D, etc) give you a probability Classically distribution in this Rolling space hopefully with D some sharp predictions Albrecht CosmoCruise 9/5/15 81
82 The multiverse of eternal inflation with multiple classical rolling directions Classically Rolling A String theory landscape even more complicated (e.g. many types of eternal inflation) Self reproduction regime Classically Rolling B Where Classically are we? Rolling Where are we? (Young universe, old universe, Expect the C theory to curvature, physical properties A, B, C, D, etc) give you a probability Classically distribution in this Rolling space hopefully with D some sharp predictions Albrecht CosmoCruise 9/5/15 82
83 Challenges for eternal inflation Anything that can happen will happen infinitely many times (A. Guth) 1) Measure Problems ( / ) 2) Problems defining probabilities 3) Problems/hidden assumptions re initial conditions problem claiming generic predictions about state cannot claim solution to cosmological problems Related to 2 nd law, low S start Albrecht CosmoCruise 9/5/15 83
84 Challenges for eternal inflation Anything that can happen will happen infinitely many times (A. Guth) 1) Measure Problems ( / ) 2) Problems defining probabilities 3) Problems/hidden assumptions re initial conditions problem claiming generic predictions about state cannot claim solution to cosmological problems Related to 2 nd law, low S start Inflation Eternal Inflation Albrecht CosmoCruise 9/5/15 84
85 Challenges for eternal inflation Anything that can happen will happen infinitely many times (A. Guth) 1) Measure Problems ( / ) 2) Problems defining probabilities 3) Problems/hidden assumptions Albrecht re and initial Phillips conditions 2014: problem claiming generic 1) All probabilities predictions about are state cannot claim solution quantum. to cosmological 2) problems Must expunge purely classical Related probabilities to 2 nd law, from low S start discussion of eternal inflation Albrecht CosmoCruise 9/5/15 85
86 An important role for Brownian motion: Uncertainty in neuron transmission times QUANTUM Brownian motion of polypeptides determines exactly how many of them are blocking ion channels in neurons at any given time. This is believed to be the dominant source of neuron transmission time uncertainties t 1ms Image from n
87 Analysis of coin flip t t f t f 2 t v h tn vh v f f 4v f d v f N ft t 0.5 v h Coin diameter Using: t 1ms v v 5 m/ s n d 0.01m h f d No Principle of indifference Albrecht CosmoCruise 9/5/15 87
88 Challenges for eternal inflation Anything that can happen will happen infinitely many times (A. Guth) 1) Measure Problems ( / ) 2) Problems defining probabilities 3) Problems/hidden assumptions Albrecht re and initial Phillips conditions 2014: problem claiming generic 1) All probabilities predictions about are state cannot claim solution quantum. to cosmological 2) problems Must expunge purely classical Related probabilities to 2 nd law, from low S start discussion of eternal inflation Possible benefit to eternal inflation Albrecht CosmoCruise 9/5/15 88
89 Challenges for eternal inflation Anything that can happen will happen infinitely many times (A. Guth) 1) Measure Problems ( / ) 2) Problems defining probabilities 3) Problems/hidden assumptions Albrecht re and initial Phillips conditions 2014: problem claiming generic 1) All probabilities predictions about are state cannot claim solution quantum. to cosmological 2) problems Must expunge purely classical Related probabilities to 2 nd law, from low S start discussion of eternal inflation Possible benefit to eternal inflation Possible discussion/surprise talk topic Albrecht CosmoCruise 9/5/15 89
90 Challenges for eternal inflation Anything that can happen will happen infinitely many times (A. Guth) 1) Measure Problems ( / ) 2) Problems defining probabilities 3) Problems/hidden assumptions re initial conditions problem claiming generic predictions about state cannot claim solution to cosmological problems Related to 2 nd law, low S start Albrecht CosmoCruise 9/5/15 90
91 But if eternal inflation produces an infinite universe surely it does not matter if the start of inflation is very improbable NO Hernley, AA & Dray 2013 AA & Sorbo 2004 Albrecht CosmoCruise 9/5/15 91
92 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 92
93 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 93
94 Length scale log(r H /R H 0 ) Inflation > radiation >matter >dark energy H 2 2 Here Here Hubble length Today In Minkowski vacuum at t= log(a/a 0 ) Scale factor Albrecht CosmoCruise 9/5/15 94
95 2.5 x Slow rolling of inflaton Self reproducing regime (dominated by quantum fluctuations): Eternal inflation/multiverse Q 4 V/M GUT Observable physics generated here Extrapolating back /M P Albrecht CosmoCruise 9/5/15 95
96 Evolution of Cosmic Length log[(r H /R H 0 )] log(a/a 0 ) Albrecht CosmoCruise 9/5/15 96
97 Evolution of Cosmic Length (zooming out) log[(r H /R H 0 )] log(a/a 0 ) Albrecht CosmoCruise 9/5/15 97
98 Evolution of Cosmic Length (zooming out) log[(r H /R H 0 )] log(a/a 0 ) Albrecht CosmoCruise 9/5/15 98
99 Evolution of Cosmic Length (zooming out) 2000 log[(r H /R H 0 )] log(a/a 0 ) 3 Albrecht CosmoCruise 9/5/15 99
100 Evolution of Cosmic Length (zooming out) log[(r H /R H 0 )] log(a/a 0 ) Albrecht CosmoCruise 9/5/15 100
101 Evolution of Cosmic Length (zooming out) x log[(r H /R H 0 )] log(a/a 0 ) Albrecht CosmoCruise 9/5/15 101
102 Evolution of Cosmic Length (zooming out) 6 x log[(r H /R H 0 )] log(a/a 0 ) x 10 4 Albrecht CosmoCruise 9/5/15 102
103 Evolution of Cosmic Length (zooming out) x 10 5 log[(r H /R H 0 )] log(a/a x ) Albrecht CosmoCruise 9/5/15 103
104 Evolution of Cosmic Length (zooming out) 6 x log[(r H /R H 0 )] log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 104
105 Evolution of Cosmic Length (zooming out) 6 x 10 5 log[(r H /R H 0 )] Q log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 105
106 Evolution of Cosmic Length (zooming out) log[(r H /R H 0 )] x Q 10 1 Not at all classical! log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 106
107 log[(r H /R H 0 )] x 10 5 Self reproduction regime 1 Q 10 1 Substantial probability of fluctuating up the potential and continuing the inflationary expansion Eternal Inflation log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 107
108 log[(r H /R H 0 )] x 10 5 Self reproduction regime 1 Q 10 1 Substantial probability of fluctuating up the potential and continuing the inflationary expansion Eternal Inflation Observable Universe log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 108
109 log[(r H /R H 0 )] x 10 5 Self reproduction regime 1 Q 10 1 Substantial probability of fluctuating up the potential and continuing the inflationary expansion Eternal Inflation Observable Universe log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 109
110 log[(r H /R H 0 )] x 10 5 Self reproduction regime 1 Q 10 In Minkowski vacuum at t= 1 Substantial probability of fluctuating up the potential and continuing the inflationary expansion Eternal Inflation log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 110
111 log[(r H /R H 0 )] x 10 5 Self reproduction regime In Minkowski vacuum at t= Substantial probability of fluctuating up the potential and continuing the inflationary expansion Eternal Inflation In the abstract: The more inflation, the more tuning (see toy model 1 10 Q debate with Guth) In practice (std picture) this tuning = belief in the Bunch Davies vacuum for 1more and more modes. Is it genius? Is it cheating? log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 111
112 log[(r H /R H 0 )] x 10 5 Self reproduction regime In Minkowski vacuum at t= Substantial probability of fluctuating up the potential and continuing the inflationary expansion Eternal Inflation In the abstract: The more inflation, the more tuning (see toy model 1 10 Q debate with Guth) In practice (std picture) this tuning = belief in the Bunch Davies vacuum for 1more and more modes. Is it genius? Is it cheating? Vs AA & Sorbo log(a/a 0 ) x 10 5 Albrecht CosmoCruise 9/5/15 112
113 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 113
114 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 114
115 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Albrecht CosmoCruise 9/5/15 115
116 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Albrecht CosmoCruise 9/5/15 116
117 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Build on initial motivation re the appeal of an equilibrium system (no initial conditions ) Albrecht CosmoCruise 9/5/15 117
118 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Build on initial motivation re the appeal of an equilibrium system (no initial conditions ) Seek the Bohr Atom of cosmology Albrecht CosmoCruise 9/5/15 118
119 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Build on initial motivation re the appeal of an equilibrium system (no initial conditions ) Seek the Bohr Atom of cosmology A counterpoint to the infinities of eternal inflation Albrecht CosmoCruise 9/5/15 119
120 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Build on initial motivation re the appeal of an equilibrium system (no initial conditions ) Seek the Bohr Atom of cosmology A counterpoint to the infinities of eternal inflation In our view, cosmologists should heed mathematician David Hilbert s warning: although infinity is needed to complete mathematics, it occurs nowhere in the physical Universe. J Silk & J. Ellis Nature (2014) Albrecht CosmoCruise 9/5/15 120
121 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Build on initial motivation re the appeal of an equilibrium system (no initial conditions ) Seek the Bohr Atom of cosmology A counterpoint to the infinities of eternal inflation Unabashedly exploit uncertainties about the fundamental physics (i.e. when continuum field theory is good, and when it breaks down) to construct a realistic cosmology Albrecht CosmoCruise 9/5/15 121
122 de Sitter Equilibrium (dse) cosmology Take ideas from Holography, Λ to construct a finite cosmology (beyond EFT) Build on initial motivation re the appeal of an equilibrium system (no initial conditions ) Seek the Bohr Atom of cosmology A counterpoint to the infinities of eternal inflation Unabashedly exploit uncertainties about the fundamental physics (i.e. when continuum field theory is good, and when it breaks down) to construct a realistic cosmology AA: arxiv: AA: arxiv: AA: arxiv: AA & Sorbo: hep th/ Albrecht CosmoCruise 9/5/15 122
123 Implications of the de Sitter horizon Maximum entropy 1 2 S A H 3 Gibbons Hawking Temperature T GH H 8 G 3 Gibbons & Hawking 1977 Albrecht CosmoCruise 9/5/15 123
124 De Sitter Space: The ultimate equilibrium for the universe? Horizon 2 1 S A H T GH H 8 G 3 Albrecht CosmoCruise 9/5/15 124
125 Implications of the de Sitter horizon Maximum entropy 1 2 S A H 3 Gibbons Hawking Temperature T GH H 8 G 3 Only a finite volume ever observed If is truly constant: Cosmology as fluctuating Eqm. Maximum entropy finite Hilbert space of S dimension N e Banks & Fischler & Dyson et al. Albrecht CosmoCruise 9/5/15 125
126 Implications of the de Sitter horizon Maximum entropy 1 2 S A H 3 Gibbons Hawking Temperature T GH H 8 G 3 Only a finite volume ever observed dse cosmology If is truly constant: Cosmology as fluctuating Eqm.?? Maximum entropy finite Hilbert space of S dimension N e Banks & Fischler & Dyson et a Albrecht CosmoCruise 9/5/15 126
127 Equilibrium Cosmology Albrecht CosmoCruise 9/5/15 127
128 Equilibrium Cosmology An eqm. theory does not require any theory of initial conditions. The probability of appearing in a given state is given entirely by stat mech, and is thus given by the dynamics. If you know the Hamiltonian you know how to assign probabilities to different states without any special theory of initial conditions. Dyson et al 2002 Albrecht CosmoCruise 9/5/15 128
129 Rare Fluctuation Albrecht CosmoCruise 9/5/15 129
130 Rare Fluctuation Albrecht CosmoCruise 9/5/15 130
131 Rare Fluctuation Small fluctuations are more likely than large ones Albrecht CosmoCruise 9/5/15 131
132 Rare Fluctuation Move Ergodicity to hidden degrees of freedom (we *know* state counting arguments do note apply to the observable universe) AA 2014 Albrecht CosmoCruise 9/5/15 132
133 Rare Fluctuation Move Ergodicity to hidden degrees of freedom (we *know* state counting arguments do note apply to the observable universe) AA 2014 Possible discussion/surprise talk topic Albrecht CosmoCruise 9/5/15 133
134 Concept: Realization: de Sitter Space Albrecht CosmoCruise 9/5/15 134
135 Rare Fluctuation Albrecht CosmoCruise 9/5/15 135
136 Fluctuating from dse to inflation: The process of an inflaton fluctuating from late time de Sittter to an inflating state is dominated by the Farhi Guth Guven (FGG) process A seed is formed from the Gibbons Hawking radiation that can then tunnel via the Guth Farhi instanton. Rate is well approximated by the rate of seed formation: ms ms TGH H e e Seed mass: m ch kg s I I GeV I 4 1/2 Albrecht CosmoCruise 9/5/15 136
137 Fluctuating from dse to inflation: The process of an inflaton fluctuating from late time de Sittter to an inflating state is dominated by the Farhi Guth Guven (FGG) process A seed is formed from the Gibbons Hawking radiation that can then tunnel via the Guth Farhi instanton. Rate is well approximated by the rate of seed formation: ms ms TGH H e e Seed mass: m ch kg s I I GeV Small seed can produce an entire universe Evade Boltzmann Brain problem I 4 1/2 Albrecht CosmoCruise 9/5/15 137
138 Fluctuating from dse to inflation: The process of an inflaton fluctuating from late time de Sittter to an inflating state is dominated by the Farhi Guth Guven (FGG) process A seed Inflation is formed plays from the Gibbons Hawking role we radiation always that can thought then tunnel it could via the Guth Farhi instanton. play: Rate is well Makes approximated a whole by universe the rate of seed formation: ms ms Seed mass: out of one easy to achieve TGH H e e fluctuation. m ch kg s I I GeV Small seed can produce an entire universe Evade Boltzmann Brain problem I 4 1/2 Albrecht CosmoCruise 9/5/15 138
139 Fluctuating from dse to inflation: The process of an inflaton fluctuating from late time de Sittter to an inflating state is dominated by the M 0 not a problem for G F Farhi Guth Guven (FGG) process process (A. Ulvestad & AA 2012) A seed is formed from the Gibbons Hawking radiation that can then tunnel See via also the Freivogel Guth Farhi et al 2006, instanton. Banks 2002 Rate is well approximated by the rate of seed formation: ms ms TGH H e e Seed mass: m ch kg s I I GeV I 4 1/2 Albrecht CosmoCruise 9/5/15 139
140 Events De Sitter like spacetime Baby Universe Eqm. Seed Fluctuation Time Tunneling Evolution Inflation Radiation Evolution Matter de Sitter & Recoupling & Equilibration Albrecht CosmoCruise 9/5/ de Sitter
141 Events De Sitter like spacetime Baby Universe Eqm. Seed Fluctuation Time Tunneling Right Evolution Timescale Evolution Inflation Radiation Matter de Sitter & Recoupling & Equilibration Albrecht CosmoCruise 9/5/ de Sitter
142 Implications of finite Hilbert space N S e Recurrences Eqm. Breakdown of continuum field theory Albrecht CosmoCruise 9/5/15 142
143 Implications of finite Hilbert space N S e Recurrences Eqm. Breakdown of continuum field theory Albrecht CosmoCruise 9/5/15 143
144 Implications of finite Hilbert space N S e Recurrences Eqm. Breakdown of continuum field theory Albrecht CosmoCruise 9/5/15 144
145 m log[l/(ch 0-1 )] I r This much inflation fills one de Sitter horizon log(a/a 0 ) Albrecht CosmoCruise 9/5/15 145
146 m log[l/(ch 0-1 )] I r This much inflation fills more than one de Sitter horizon, generating log(a/atotal 0 ) entropy SMax S and affecting regions beyond the horizon of the observer Albrecht CosmoCruise 9/5/15 146
147 10 log[l/(ch 0-1 )] In dse cosmology this region is unphysical. Breakdown of effective field theory prevents inflation from filling more than one de Sitter horizon m I r log(a/a 0 ) Albrecht CosmoCruise 9/5/15 147
148 10 log[l/(ch 0-1 )] In dse cosmology this region is unphysical. Breakdown of effective field theory prevents inflation from filling more than one de Sitter horizon m I r log(a/a Equivalent 0 ) to Banks Fischler holographic constraint on number of e foldings of inflation (D Phillips & AA in prep) Albrecht CosmoCruise 9/5/15 148
149 2.5 x V/M GUT To get eternal inflation, we made what we thought was a simple extrapolation, but wound up with a highly problematic theory Q /M P Albrecht CosmoCruise 9/5/15 149
150 4 V/M GUT 2.5 x 104 dse: The extrapolation that leads to eternal inflation is naïve, in that it neglects the breakdown 2 of effective field theory. dse uses holographic arguments to estimate this breakdown Q Breakdown of effective field theory (extrapolation invalid) /M P Albrecht CosmoCruise 9/5/15 150
151 Fluctuating from dse to inflation: The process of an inflaton fluctuating from late time de Sittter to an inflating state is dominated by the Farhi Guth Guven (FGG) process A seed is formed from the Gibbons Hawking radiation that can then tunnel via the Guth Farhi instanton. Rate is well approximated by the rate of seed formation ms ms Seed mass: TGH H e e m ch kg s I I GeV I 4 1/2 I Large exponentially favored saturation of dse bound Albrecht CosmoCruise 9/5/15 151
152 10 log[l/(ch 0-1 )] dse bound on inflation given by past horizon log(a/a 0 ) Albrecht CosmoCruise 9/5/15 152
153 10 log[l/(ch 0-1 )] dse bound on inflation given by past horizon A variety of inflation models, all saturating the dse bound log(a/a 0 ) Albrecht CosmoCruise 9/5/15 153
154 log[l/(ch 0-1 )] Evolution of curvature radius Curvature radius set by initial curvature B k c H k a A variety of inflation models, all saturating the dse bound log(a/a 0 ) Albrecht CosmoCruise 9/5/15 154
155 k k 0 k log[l/(ch 0-1 )] c H H Curvature radius set by initial curvature 2 R H R 0 k Evolution of curvature radius 2 B k is given by this gap c H k a A variety of inflation models, all saturating the dse bound log(a/a 0 ) Albrecht CosmoCruise 9/5/15 155
156 log[l/(ch 0-1 )] AA: arxiv: log(a/a 0 ) Albrecht CosmoCruise 9/5/15 156
157 dse Cosmology and cosmic curvature The Guth Farhi process starts inflation with an initial curvature set by the curvature of the B Guth Farhi bubble k Inflation dilutes the curvature, but dse cosmology has a minimal amount of inflation Albrecht CosmoCruise 9/5/15 157
158 Predicted k from dse cosmology is: Independent of almost all details of the cosmology Just consistent with current observations Will easily be detected by future observations k B k B k B k m / B k Albrecht CosmoCruise 9/5/15 158
159 Predicted k from dse cosmology is: Independent of almost all details of the cosmology Just consistent with current observations Will easily be detected by future observations k B k B k B k m / B k Albrecht CosmoCruise 9/5/15 159
160 Predicted k from dse cosmology is: Independent of almost all details of the cosmology Just consistent with current observations Will easily be detected by future observations k B k B k B k 0.1 Don t assume curvature = 0! 0 m / B k Albrecht CosmoCruise 9/5/15 160
161 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 161
162 Outline 1. Introduction 2. Tuning & Entropy 3. Temporal Provincialism 4. Eternal Inflation, measures and probabilities 5. The Bunch Davies vacuum 6. de Sitter equilibrium cosmology 7. Conclusions Albrecht CosmoCruise 9/5/15 162
163 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics Albrecht CosmoCruise 9/5/15 163
164 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics Starobinsky talk Albrecht CosmoCruise 9/5/15 164
165 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics 2) Questions of what went before, tuning, measures etc are tough ones. The ability of inflation theory (or any other theory) to provide deep insights into these is unclear. Albrecht CosmoCruise 9/5/15 165
166 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics 2) Questions of what went before, tuning, measures etc are tough ones. The ability of inflation theory (or any other theory) to provide deep insights into these is unclear. 3) Ability of inflation to map common beliefs about the vacuum onto observable facts about the universe is cute/deep/shallow in relation to 1 & 2 Albrecht CosmoCruise 9/5/15 166
167 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics 2) Questions of what went before, tuning, measures etc are tough ones. The ability of inflation theory (or any other theory) to provide deep insights into these is unclear. 3) Ability of inflation to map common beliefs about the vacuum onto observable facts about the universe is cute/deep/shallow in relation to 1 & 2 4) These questions have an important role in stimulating the next level of progress in cosmology and fundamental physics. Albrecht CosmoCruise 9/5/15 167
168 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics 2) Questions of what went before, tuning, measures etc are tough ones. The ability of inflation theory (or any other theory) to provide deep insights into these is unclear. 3) Ability of inflation to map common beliefs about the vacuum onto observable facts about the universe is cute/deep/shallow in relation to 1 & 2 4) These questions have an important role in Inflation stimulating the next level of progress in cosmology and fundamental solves the physics. cosmological puzzles Albrecht CosmoCruise 9/5/15 168
169 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics 2) Questions of what went before, tuning, measures etc are tough ones. The ability of inflation theory (or any other theory) to provide deep insights into these is unclear. 3) Ability of inflation to map common beliefs about the vacuum onto observable facts about the universe is cute/deep/shallow in relation to 1 & 2 4) These questions have an important role in Inflation stimulating the next level of progress in cosmology and fundamental solves the physics. cosmological puzzles Albrecht CosmoCruise 9/5/15 169
170 Concluding thoughts 1) O(60) e folds of inflation make a great tool for understanding the cosmos and linking it with particle physics 2) Questions of what went before, tuning, measures etc are tough ones. The ability of inflation theory (or any other theory) to provide deep insights into these is unclear. 3) Ability of inflation to map common beliefs about the vacuum onto observable facts about the universe is cute/deep/shallow in relation to 1 & 2 4) These questions have an important role in stimulating the next level of progress in cosmology and fundamental physics. 5) Further progress will not be made using simply EFTs (thus dse) Albrecht CosmoCruise 9/5/15 170
171 How do ideas of dse impact my research in practical terms: Search for finite quantum theory that looks approximately like de Sitter interior with finite thermal horizon (hard) Work on de Sitter equilibration Work on short inflation phenomenology. Albrecht CosmoCruise 9/5/15 171
172 1. Transients in finite inflation Andrew Scacco, Andreas Albrecht arxiv: Holographic bounds and finite inflation Daniel Phillips, Andrew Scacco, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Equilibration of a quantum field in de Sitter space time Andreas Albrecht (UC, Davis), R. Holman (Carnegie Mellon U.), Benoit J. Richard (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Cosmological Consequences of Initial State Entanglement Andreas Albrecht, Nadia Bolis (UC, Davis), R. Holman (Carnegie Mellon U.). JHEP 1411 (2014) 09 arxiv: No Firewalls or Information Problem for Black Holes Entangled with Large Systems Henry Stoltenberg, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 2, arxiv: Eternal Inflation with Arrival Terminals Henry Stoltenberg, Andreas Albrecht (UC, Davis) Phys.Rev. D91 (2015) 2, arxiv: Albrecht CosmoCruise 9/5/15 172
173 1. Transients in finite inflation Andrew Scacco, Andreas Albrecht arxiv: Impressive students applying for jobs this fall 3. Holographic bounds and finite inflation Daniel Phillips, Andrew Scacco, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Equilibration of a quantum field in de Sitter space time Andreas Albrecht (UC, Davis), R. Holman (Carnegie Mellon U.), Benoit J. Richard (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Cosmological Consequences of Initial State Entanglement Andreas Albrecht, Nadia Bolis (UC, Davis), R. Holman (Carnegie Mellon U.). JHEP 1411 (2014) 09 arxiv: No Firewalls or Information Problem for Black Holes Entangled with Large Systems Henry Stoltenberg, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 2, arxiv: Eternal Inflation with Arrival Terminals Henry Stoltenberg, Andreas Albrecht (UC, Davis) Phys.Rev. D91 (2015) 2, arxiv: Albrecht CosmoCruise 9/5/15 173
174 1. Transients in finite inflation Andrew Scacco, Andreas Albrecht arxiv: Impressive students applying for jobs this fall 3. Holographic bounds and finite inflation Daniel Phillips, Andrew Scacco, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Equilibration of a quantum field in de Sitter space time Andreas Albrecht (UC, Davis), R. Holman (Carnegie Mellon U.), Benoit J. Richard (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Cosmological Consequences of Initial State Entanglement Andreas Albrecht, Nadia Bolis (UC, Davis), R. Holman (Carnegie Mellon U.). JHEP 1411 (2014) 09 arxiv: No Firewalls or Information Problem for Black Holes Entangled with Large Systems Henry Stoltenberg, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 2, arxiv: Eternal Inflation with Arrival Terminals Henry Stoltenberg, Andreas Albrecht (UC, Davis) Phys.Rev. D91 (2015) 2, arxiv: Impressive students here at cosmocruise Albrecht CosmoCruise 9/5/15 174
175 1. Transients in finite inflation Andrew Scacco, Andreas Albrecht arxiv: Impressive students applying for jobs this fall 3. Holographic bounds and finite inflation Daniel Phillips, Andrew Scacco, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Equilibration of a quantum field in de Sitter space time Andreas Albrecht (UC, Davis), R. Holman (Carnegie Mellon U.), Benoit J. Richard (UC, Davis). Phys.Rev. D91 (2015) 4, arxiv: Cosmological Consequences of Initial State Entanglement Andreas Albrecht, Nadia Bolis (UC, Davis), R. Holman (Carnegie Mellon U.). JHEP 1411 (2014) 09 arxiv: Next talk 6. No Firewalls or Information Problem for Black Holes Entangled with Large Systems Henry Stoltenberg, Andreas Albrecht (UC, Davis). Phys.Rev. D91 (2015) 2, arxiv: Eternal Inflation with Arrival Terminals Henry Stoltenberg, Andreas Albrecht (UC, Davis) Phys.Rev. D91 (2015) 2, arxiv: Impressive students here at cosmocruise Albrecht CosmoCruise 9/5/15 175
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