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Fluid equations for fast-moving electroweak bubble walls
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The cosmological electroweak phase transition can be strongly first order in extended particle physics models. To accurately predict the speed and shape of the bubble walls during such a transition, Boltzmann equations for the CP-even fluid perturbations must be solved. We point out that the equations usually adopted lead to unphysical behavior of the perturbations, for walls traveling close to or above the speed of sound in the plasma. This is an artifact that can be overcome by more carefully truncating the full Boltzmann equation. We present an improved set of fluid equations, suitable for studying the dynamics of both subsonic and supersonic walls, of interest for gravitational wave production and electroweak baryogenesis.
Forward citations
Cited by 4 Pith papers
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A new matching condition that includes entropy production reveals that fast detonation bubble walls and slower deflagration walls can both be stable, with the fast solution typically winning in practice.
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The fluid-Ansatz and WallGo methods agree for mild phase transitions but diverge by tens of percent for strong ones, where the semi-classical approximation itself may break down.
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Thermal Masses and Bubble-Wall Friction in Cosmological Phase Transitions
Including thermal masses in both the Boltzmann source and collision terms removes the infrared gauge-boson enhancement, making W-boson friction subleading in the singlet-extended Standard Model.
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The First Particles
No new result: the paper is an expository review of reheating, electroweak baryogenesis, and leptogenesis in early universe cosmology.
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