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Relativistic bubble collisions -- a closer look
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Relativistic bubble collisions -- a closer look
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We study scalar bubble collisions in first-order phase transitions focusing on the relativistic limit. We propose 'trapping equation' which describes the wall behavior after collision, and test it with numerical simulations in several setups. We also examine the energy dynamics after collision and discuss its implications to gravitational wave production.
Forward citations
Cited by 6 Pith papers
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Particle production from bubble collisions
Heavy particles are produced in bubble-wall collisions by on-shell partonic scatterings, not by off-shell decay of the classical field, so the earlier rates and their phenomenological signals are parametrically overestimated.
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Can the universe be matter-dominated after a supercooled first-order phase transition?
After a supercooled first-order phase transition, the scalar field's equation of state is set by the bubble-wall Lorentz factor γ*, and matter domination is delayed until a/a* ≃ γ* in the free-streaming limit.
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Particle productions during collisions of highly boosted bubble walls
Bubble-wall collisions produce ultra-heavy particles with a universal spectrum ∝ [V'(2vφ)]²/χ⁴, localized at the collision instant.
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New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions
Defines peak-integrated sensitivity curves (PISCs) that fold in the expected spectral shape of gravitational waves from cosmological phase transitions and supplies semianalytical fits plus public data for major detectors.
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Tunnelling out of Starobinsky inflation: Raising the spectral tilt
A first-order phase-transition exit from a displaced Starobinsky branch truncates ~12 e-folds, shifting the spectral tilt from n_s≈0.965 to ≈0.973 at r≈2×10⁻³.
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Dark Matter Production from Bubble Collisions during a First-Order Phase Transition at the End of Inflation
Bubble collisions during a first-order phase transition at the end of inflation can generate the observed dark matter abundance in a restricted region of parameter space via direct production and spectator decays.
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