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The cosmological electroweak phase transition can be strongly first order inextended particle physics models. To accurately predict the speed and shape ofthe bubble walls during such a transition, Boltzmann equations for the CP-evenfluid perturbations must be solved. We point out that the equations usuallyadopted lead to unphysical behavior of the perturbations, for walls travelingclose to or above the speed of sound in the plasma. This is an artifact thatcan be overcome by more carefully truncating the full Boltzmann equation. Wepresent an improved set of fluid equations, suitable for studying the dynamicsof both subsonic and supersonic walls, of interest for gravitational waveproduction and electroweak baryogenesis.

Fluid equations for fast-moving electroweak bubble walls