Cosmological Energy Budget of Cosmological First Order Phase - PowerPoint PPT Presentation

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

Why Bubbles Motivation: Why Bubbles ? Cosmological First Order Phase Transitions Electroweak Electroweak  Phase Transition Phase Transition Nucleation & Growth of Bubbles Gravitational waves Gravitational waves Baryogenesis Baryogenesis Courtesy of David Weir Bubble Collisions & (anisotropic) Plasma Motions Produce Stochastic Gravitational Wave Signature Could be Detected by LISA L arge I nterferometer S pace A ntenna Bubble Expansion & Interaction w. Plasma Can Yield Baryogenesis 1

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

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

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

Dynamics of Thermal Plasma Looking Far from the Phase Boundary: Fluid Motion Fluid Motion Self - Similar Ansatz  Fluid MOTION = 0.577... Plasma Speed of Sound   Fluid TEMPERATURE 5

Dynamics of Thermal Plasma Looking Far from the Phase Boundary: Fluid Motion Fluid Motion Self - Similar Ansatz  Fluid MOTION = 0.577... Plasma Speed of Sound   Fluid TEMPERATURE + Fluid Velocity Eq. Matching Conditions on Bubble Wall Boundary conditions Solutions Solutions for Fluid Motion for Fluid Motion ”Bubble Expansion Modes” 5

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

Dynamics of Thermal Plasma Solutions for Fluid Motion S upersonic DEtonations DEtonations F luid at Rest in F ront of W all R arefaction W ave B ehind W all S ubsonic DEflagrations DEflagrations F luid at Rest B ehind W all C ompression W ave in F ront of W all E nds in a S hock F ront S upersonic hybrids hybrids B oth C ompression & R arefaction W aves 7

Dynamics of Thermal Plasma Solutions for Fluid Motion For = cte Continuous Evolution Deflagrations  hybrids  detonations Deflagrations  hybrids  detonations as v w Increases 8

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

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

Energy Budget of the Phase Transition Energy Liberated During the Phase Transition Acts as Source of Gravitational Waves Bubbles Expanding in Vacuum Perfect Conversion of Liberated Energy into Kinetic Energy Bubbles Expanding in Thermal Plasma NOT Perfect Conversion of Liberated Energy into Kinetic Energy Efficiency Factor Depends on T N , v W , α 10

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

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

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

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

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

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) 3854-3868 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) 124025 C. Caprini and J. M. No, JCAP 1201:031 (2012)

Probing the EW Epoch with GW GW Bubble soUrces GW Bubble soUrces Sound Waves Sound Waves Hindmarsh, Huber, Rummukainen, Weir, Phys. Rev. Lett 112 (2014) 041301 Courtesy of D. Weir (Stavanger) Courtesy of D. Weir (Stavanger) Turbulence Turbulence Caprini, Durrer, Servant, JCAP 0912 (2009) 024 ϵ (Stochastic) GW Signal Detectable by LISA ! !

(e)LISA As of Sept. 2016 3 rd Arm 3 rd Arm 2-5 2-5 The Next/Future step The Next/Future step on its way! on its way! Gravitational Wave Astronomy in Space (success of eLISA Pathfinder) (success of eLISA Pathfinder) LISA L arge I nterferometer S pace A ntenna

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