Energy Budget of Cosmological First Order Phase Transitions

Transcription

1 Energy Budget Cosmological First Order Phase Transitions Jose Miguel No King's College London Making the EW Phase Transition (Theoretically) Strong

2 Motivation: Why Bubbles? Cosmological First Order Phase Transitions Electroweak Nucleation Gravitational waves Phase Transition & Growth Bubbles Baryogenesis Courtesy David Weir Bubble Collisions & (anisotropic) Plasma Motions Produce Stochastic Gravitational Wave Signature Could be Detected by LISA Large Interferometer Space Antenna Bubble Expansion & Interaction w. Plasma Can Yield Baryogenesis 1

3 Dynamics Thermal Plasma Expanding Bubbles Perturb Thermal Plasma =0 =v Close to Phase Boundary Bubble Wall =0 V =v + V T + T Far from Phase Boundary Energy-Momentum Conservation - - 2

4 Dynamics Looking Closely Thermal Plasma at the Phase Boundary: matching Across Bubble wall Bubble Wall =0 V + =v V Perfect Fluid - Energy-Momentum Conservation T + T Across Bubble Wall - + Steady State Bubble Expansion Wall Reference Frame Simple Ansatz for Fluid E.O.S. (Bag E.O.S. ) 3

5 Dynamics Thermal Plasma Looking Closely at the Phase Boundary: matching Across Bubble wall Bubble Wall =0 V =v + V T + T - - ➊ Wall Reference Frame Two Branches Solutions ➋ ➊ ➋ ( Only if ) 4

6 Dynamics Looking Far Thermal Plasma from the Phase Boundary: Fluid Motion Self-Similar Ansatz Fluid MOTION = Plasma Speed Sound Fluid TEMPERATURE 5

7 Dynamics Looking Far Thermal Plasma from the Phase Boundary: Fluid Motion Self-Similar Ansatz Fluid MOTION = Plasma Speed Sound Fluid TEMPERATURE Fluid Velocity Eq. + Matching Conditions on Bubble Wall Solutions for Fluid Motion Boundary conditions Bubble Expansion Modes 5

8 Dynamics Looking Far Thermal Plasma from the Phase Boundary: Fluid Motion Inspecting Is Single Valued Function 6

9 Dynamics Solutions Thermal Plasma for Fluid Motion Supersonic DEtonations Fluid at Rest in Front Wall Rarefaction Wave Behind Wall Subsonic DEflagrations Fluid at Rest Behind Wall Compression Wave in Front Wall Ends in a Shock Front hybrids Supersonic Both Compression & Rarefaction Waves 7

10 Dynamics Solutions For Thermal Plasma for Fluid Motion = cte Continuous Evolution as vw Increases Deflagrations hybrids detonations 8

11 Dynamics Collection Thermal Plasma Relevant Effects... DEflagrations Slow Moving Bubbles Good for Baryogenesis DEtonations Fast Moving Bubbles Bad(?) for Baryogenesis Local Symmetry Restoration 9

12 Energy Budget Energy Liberated During Gravitational Waves the the Phase Transition Phase Transition Acts as Source Bubbles Expanding in Vacuum Perfect Conversion Liberated Energy into Kinetic Energy Bubbles Expanding in Thermal Plasma NOT Perfect Conversion Liberated Energy into Kinetic Energy Efficiency Factor 10

13 Energy Budget Energy Liberated During the the Gravitational Waves Phase Transition Phase Transition Acts as Source Bubbles Expanding in Vacuum Perfect Conversion Liberated Energy into Kinetic Energy Bubbles Expanding in Thermal Plasma NOT Perfect Conversion Liberated Energy into Kinetic Energy Efficiency Factor Depends on TN, vw, α 10

14 Energy Budget the Phase Transition Controls Energy Budget Energy not transformed into plasma bulk motion ( 1- ) used to increase plasma thermal energy 11

15 Energy Budget the Phase Transition Controls Energy Budget Energy not transformed into plasma bulk motion ( 1- ) used to increase plasma thermal energy 11

16 Energy Budget the Phase Transition Gravitational Wave Amplitude Depends Quadratically on e.g. Sound Waves as GW Source 12

17 Energy Budget the Phase Transition Gravitational Wave Amplitude Depends Quadratically on e.g. Sound Waves as GW Source 12

18 Energy Budget the Phase Transition Gravitational Wave Amplitude Depends Quadratically on e.g. Sound Waves as GW Source 12

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20 References Bubble Expansion Solutions P. J. Steinhardt, Phys. Rev. D 25 (1982) 2074 M. Laine, Phys. Rev. D 49 (1994) 3847 J. Ignatius, K. Kajantie, H. Kurki-Suonio and M. Laine, Phys. Rev. D 49 (1994) H. Kurki-Suonio and M. Laine, Phys. Rev. D 51 (1995) 5431 Efficiency Coefficients Energy Budget M. Kamionkowski, A. Kosowsky and M. S. Turner, Phys. Rev. D 49 (1994) 2837 J. R. Espinosa, T. Konstandin, J. M. No. and G. Servant, JCAP 1006:028 (2010) Implications for Baryogenesis J. M. No, Phys. Rev. D 84 (2011) C. Caprini and J. M. No, JCAP 1201:031 (2012)

21 Probing the EW Epoch with GW GW Bubble sources Sound Waves Hindmarsh, Huber, Rummukainen, Weir, Phys. Rev. Lett 112 (2014) Courtesy D. Weir (Stavanger) Turbulence Caprini, Durrer, Servant, JCAP 0912 (2009) 024 ϵ (Stochastic) GW Signal Detectable by LISA!

22 (e)lisa As Sept rd Arm 2-5 The Next/Future step Gravitational Wave Astronomy in Space LISA L arge I nterferometer S pace A ntenna on its way! (success elisa Pathfinder)

23 Probing the EW Epoch with GW LISA Sensitivity to BSM Caprini et al, JCAP 1604 (2016) 001 for the (e) LISA Cosmology Working Group