Standard Model Thermodynamics: Effect on Gravitational Wave and Dark Matter
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1 Standard Model Thermodynamics: Effect on Gravitational Wave and Dark Matter Satoshi Shirai (Kavli IPMU) based on Ken'ichi Saikawa and SS,
2 Remnant of Early Universe The present Universe is made of relic from early Universe: Baryon, dark matter, radiation Once generated, it evolves to today. Dilution. Redshift. Decay. Self-annihlation. Interaction with thermal plasma. 2
3 Thermal History Inflation EW PT QCD PT ~ 100 GeV ~ 100 MeV BBN, Neutrino DC ~ 1 MeV time 3
4 Thermal History Inflation EW PT QCD PT ~ 100 GeV ~ 100 MeV Something generated BBN, Neutrino DC ~ 1 MeV Observed time 4
5 Precision Cosmology Planck Ultimate Decigo (far future GW detector) 5
6 Cosmic Evolution (Friedmann equation) (entropy conservation) 6
7 Goal Updating by using the Higgs and latest lattice QCD Plus: updating some non-thermal contributions: e.g., neutrino and photon decoupling Clarify the present uncertainties Study effect on physical observables: gravitational wave and WIMP dark matter 7
8 Contents 1. Introduction 2. Gravitational Wave evolution of GW relation with equation of state 3. WIMP Dark Matter 4. Summary 8
9 Graviational Wave 9
10 Gravitational Wave Astronomy 10
11 Look into the distance CMB scatter surface Source Propagation CMB enjoys cosmic evolution Rich information on source and background 11
12 Look into the distance CMB scatter surface GW source 12
13 Look into the distance GW can penetrate plasm Information of very far object Physics at high energy GW source 13
14 GW Sources and propagation Astrophysical origins (star binary, super nova, ) Phase transition (QCD, Electroweak?) Inflation 14
15 GW from Inflation inflation = Start of Universe GW affected in propagation GW from inflation knows whole history of Universe 15
16 Evolution of GW 16
17 Basic Equation Source term Transfer function: how GW propagates 17
18 Rough Picture of Evolution Inflation Radiation Matter GW Frozen Evolution horizon crossing 18
19 Seto and Yokoyama, gr-qc/ Evolution after HC Equation of state 19
20 Examples radiation dominant era matter dominant era GW in radiation era is constant and diluted in matter era 20
21 Spectrum matter dom. radiation dom. Earlier horizon crossing 21
22 Radiation era 22
23 Horizon Crossing matter dom. radiation dom. Earlier horizon crossing 23
24 Spectrum 24
25 Spectrum MD RD 25
26 Standard Model for precision of GW 26
27 Thermodynamics of SM Watanabe and Komatsu astro-ph/ So far, GW calculation based on ideal gas picture All SM particles are interacting: never ideal gas 27
28 Thermodynamics of SM Non-thermal process Neutrino and photon decoupling Non-perturbation QCD phase transition EW phase transition Perturbation EW and QCD interaction 28
29 State of Art Neutrino decoupling (Salas and Pastor, ) thermal QED, neutrino oscillation QCD phase transition (Borsanyi et.al, ) (2+1+1) flavor lattice, physical mass EW phase transition (D Onofrio and Rummukainen, ) 125 GeV Higgs with lattice Perturbation (Kajantie et.al, hep-ph/ ) hard thermal loop, gs6log(gs) 29
30 Photon and Lepton Neutrino decoupling (Salas and Pastor, ) thermal QED, neutrino oscillation We add hadron and muon contribution and estimate entropy 30
31 QCD Cross Over 31
32 QCD perturbation ?+0.5 higher-loop leads to alpha3 contribution: Linde problem Linde, Phys. Lett. B96, 289 (1980) 32
33 EWPT on Lattice D Onofrio and Rummukainen,
34 Connecting two regions Connecting by using perturbation expressions: 34
35 Result of geff 35
36 Comparison with other works 36
37 Result 37
38 QCD region 38
39 High-energy region Expected error bar of ultimate DECIGO with instrumental and self noise 39
40 Neutrino and Photon Free-Streaming Present / old result neutrino free-streaming photon free-streaming 40
41 Summary of GW Update by using EW and QCD lattice result Interpolate with perturbation result (Free-streaming effect of neutrino and photon improved) f ~10-8 Hz (QCD era) is significantly modified Even T>>TeV scale, geff is smaller by O(1)%, compared to ideal gas case 41
42 WIMP DM 42
43 WIMP Dark Matter Weakly Interacting Massive Particle DM abundance DM Standard Model (SM) particle DM SM 500 GeV DM Time 43
44 Boltzmann Equation 44
45 S-wave annihilating DM 45
46 Comparison 46
47 Summary Basically we have O(1)% uncertainty geff Many cosmological observables suffer from this error Need to improve estimation of SM thermodynamics in light of precision cosmology You can get data and fitting formula of EOS and GW 47
We can check experimentally that physical constants such as α have been sensibly constant for the past ~12 billion years
² ² ² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical observations ² Dark matter: relic particles ² Dark matter:
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