preheating THE UNIVERSE (Some New Aspects)

Transcription

1 preheating THE UNIVERSE (Some New Aspects) DANIEL G. FIGUEROA HELSINKI UNIVERSITY (HU) & HELSINKI INSTITUTE of PHYSICS (HIP) August 22-26, COSMO 2011 CAUP, Porto, Portugal, Europe, Earth, Solar System, Universe

2 PHYSICAL CONTEXT: REHEATING INFLATION REHEATING BIG BANG THEORY

3 PHYSICAL CONTEXT: REHEATING INFLATION REHEATING BIG BANG THEORY

4 IMPROVING UNDERSTANDING of REHEATING (2 ways) 1 Poor Understanding of RH: ABSENCE: SM, DM, Thermalization,... DIFFICULTIES: Non-Lin, Non-Pert, Out-of-Eq. 2 ( PHENOMENOLOGICAL APPROACH: ) Phenomenological effects with observable consequences Gravitational Waves Production Non Gaussianity in Matter Density Perturbations Baryogenesis Mechanisms 3 THEORETICAL APPROACH: Embedding into Gauge Framework Adding Fermions Identify Fields with SM dof (and DM) Study Thermalization

5 IMPROVING UNDERSTANDING of REHEATING (2 ways) 1 Poor Understanding of RH: ABSENCE: SM, DM, Thermalization,... DIFFICULTIES: Non-Lin, Non-Pert, Out-of-Eq. 2 ( PHENOMENOLOGICAL APPROACH: ) Phenomenological effects with observable consequences Gravitational Waves Production Non Gaussianity in Matter Density Perturbations Baryogenesis Mechanisms 3 THEORETICAL APPROACH: Embedding into Gauge Framework Adding Fermions Identify Fields with SM dof (and DM) Study Thermalization

6 IMPROVING UNDERSTANDING of REHEATING (2 ways) 1 Poor Understanding of RH: ABSENCE: SM, DM, Thermalization,... DIFFICULTIES: Non-Lin, Non-Pert, Out-of-Eq. 2 ( PHENOMENOLOGICAL APPROACH: ) Phenomenological effects with observable consequences Gravitational Waves Production Non Gaussianity in Matter Density Perturbations Baryogenesis Mechanisms 3 THEORETICAL APPROACH: Embedding into Gauge Framework Adding Fermions Identify Fields with SM dof (and DM) Study Thermalization

7 Improving Reheating: Including the SM dof preheating WITHIN THE STANDARD MODEL dof: COMBINED preheating MECHANISM

8 preheating after HIGSS-INFLATION SM + GR + NON-MINIMAL COUPLING:

9 preheating after HIGSS-INFLATION SM + GR + NON-MINIMAL COUPLING:

10 Reheating the SM: Non-Perturbative Effects

11 Reheating the SM: Non-Perturbative Effects

12 Reheating the SM: Non-Perturbative Effects

13 Reheating the SM: Non-Perturbative Effects

14 Reheating the SM: Non-Perturbative Effects

15 Reheating the SM: Perturbative Effects

16 Reheating the SM: Perturbative Effects

17 Reheating the SM: Perturbative Effects

18 Reheating the SM: Perturbative Effects

19 Reheating the SM: Perturbative Effects

20 Reheating the SM: Perturbative Effects

21 preheating after HIGGS-INFLATION:Combined Reheating

22 preheating with many DOF: Combined Reheating IS THIS PARTICULAR TO HIGGS-INFLATION?? NO!: It is GENERIC to REHEATING with MANY DOF!

23 preheating with many DOF: Combined Reheating Inflaton Children Grand-Children Φ g 2 χ h 2 Ψ Non-Perturbative Perturbative

24 preheating with many DOF: Combined Reheating Inflaton Children Grand-Children Φ g 2 χ h 2 Ψ Non-Perturbative Perturbative ρ χ ρ Φ (j) = Fraction Energy Transferred per zero Crossing(Φ χ) t dec (j) Γ 1 j Decaying time [t j, t j+1 ](χ Ψ)

25 preheating with many DOF: Combined Reheating Inflaton Children Grand-Children Φ g 2 χ h 2 Ψ Non-Perturbative Perturbative

26 preheating with many DOF: Combined Reheating Inflaton Children Grand-Children Φ g 2 χ h 2 Ψ Non-Perturbative Perturbative

27 preheating with many DOF: Combined Reheating Inflaton Children Grand-Children Φ g 2 χ h 2 Ψ Non-Perturbative Perturbative

28 preheating after MSSM-INFLATION:Combined Reheating Allahverdi et al. 2006,2011: MSSM-Flat Direction (LLe) = Inflaton

29 preheating after MSSM-INFLATION:Combined Reheating Allahverdi et al. 2006,2011: MSSM-Flat Direction (LLe) = Inflaton

30 Improving Reheating: Including the SM dof IS THIS ALL, COMBINED (p)reheating?? NO BACKREACTION, (Re)SCATTERING, THERMALIZATION MODEL DEPENDENT!!!

31 BackReaction in HIGGS-INFLATION Reheating

32 BackReaction in HIGGS-INFLATION Reheating

33 BackReaction in MSSM-INFLATION Reheating

34 Reheating from the SM: Summary 1 Realistic Scenarios with Many dof: Combined Mechanism mixing Non-Perturbative Production + Perturbative Decays 2 Depending on the couplings/model: Param. Resonance, Mix nonp/p Effects, Instant Preheating, Inefficient, MSSM Preheating 3 Backreation, ReScattering and Thermalization specific Models 4 Higgs-Inflation: Efficient Reheating after 100 osc.: Param. Resonance initially blocked, later active. Backreaction important. 5 MSSM-Inflation: Efficient Reheating achieved after 20 oscillations Backreaction is negligible, Thermalization (T rh 10 8 GeV) 6 MORE: JUAN s TALK on FRI. / THANKS 4 YOUR ATTENTION!!!

35 Reheating from the SM: Summary 1 Realistic Scenarios with Many dof: Combined Mechanism mixing Non-Perturbative Production + Perturbative Decays 2 Depending on the couplings/model: Param. Resonance, Mix nonp/p Effects, Instant Preheating, Inefficient, MSSM Preheating 3 Backreation, ReScattering and Thermalization specific Models 4 Higgs-Inflation: Efficient Reheating after 100 osc.: Param. Resonance initially blocked, later active. Backreaction important. 5 MSSM-Inflation: Efficient Reheating achieved after 20 oscillations Backreaction is negligible, Thermalization (T rh 10 8 GeV) 6 MORE: JUAN s TALK on FRI. / THANKS 4 YOUR ATTENTION!!!

36 Reheating from the SM: Summary 1 Realistic Scenarios with Many dof: Combined Mechanism mixing Non-Perturbative Production + Perturbative Decays 2 Depending on the couplings/model: Param. Resonance, Mix nonp/p Effects, Instant Preheating, Inefficient, MSSM Preheating 3 Backreation, ReScattering and Thermalization specific Models 4 Higgs-Inflation: Efficient Reheating after 100 osc.: Param. Resonance initially blocked, later active. Backreaction important. 5 MSSM-Inflation: Efficient Reheating achieved after 20 oscillations Backreaction is negligible, Thermalization (T rh 10 8 GeV) 6 MORE: JUAN s TALK on FRI. / THANKS 4 YOUR ATTENTION!!!

37 Reheating from the SM: Summary 1 Realistic Scenarios with Many dof: Combined Mechanism mixing Non-Perturbative Production + Perturbative Decays 2 Depending on the couplings/model: Param. Resonance, Mix nonp/p Effects, Instant Preheating, Inefficient, MSSM Preheating 3 Backreation, ReScattering and Thermalization specific Models 4 Higgs-Inflation: Efficient Reheating after 100 osc.: Param. Resonance initially blocked, later active. Backreaction important. 5 MSSM-Inflation: Efficient Reheating achieved after 20 oscillations Backreaction is negligible, Thermalization (T rh 10 8 GeV) 6 MORE: JUAN s TALK on FRI. / THANKS 4 YOUR ATTENTION!!!

38 Reheating from the SM: Summary 1 Realistic Scenarios with Many dof: Combined Mechanism mixing Non-Perturbative Production + Perturbative Decays 2 Depending on the couplings/model: Param. Resonance, Mix nonp/p Effects, Instant Preheating, Inefficient, MSSM Preheating 3 Backreation, ReScattering and Thermalization specific Models 4 Higgs-Inflation: Efficient Reheating after 100 osc.: Param. Resonance initially blocked, later active. Backreaction important. 5 MSSM-Inflation: Efficient Reheating achieved after 20 oscillations Backreaction is negligible, Thermalization (T rh 10 8 GeV) 6 MORE: JUAN s TALK on FRI. / THANKS 4 YOUR ATTENTION!!!

39 Reheating from the SM: Summary 1 Realistic Scenarios with Many dof: Combined Mechanism mixing Non-Perturbative Production + Perturbative Decays 2 Depending on the couplings/model: Param. Resonance, Mix nonp/p Effects, Instant Preheating, Inefficient, MSSM Preheating 3 Backreation, ReScattering and Thermalization specific Models 4 Higgs-Inflation: Efficient Reheating after 100 osc.: Param. Resonance initially blocked, later active. Backreaction important. 5 MSSM-Inflation: Efficient Reheating achieved after 20 oscillations Backreaction is negligible, Thermalization (T rh 10 8 GeV) 6 MORE: JUAN s TALK on FRI. / THANKS 4 YOUR ATTENTION!!!

40 Back Slides BACK SLIDES

41 BackReaction in HIGGS-INFLATION Reheating

42 BackReaction in HIGGS-INFLATION Reheating

43 BackReaction in HIGGS-INFLATION Reheating