Dark Matter Production from Bubble Collisions during a First-Order Phase Transition at the End of Inflation

TL;DR

This paper investigates whether bubble collisions during a first-order phase transition at the end of inflation can produce the observed dark matter abundance, identifying viable parameter regions for this mechanism.

Contribution

It introduces a model where dark matter is generated from bubble collisions in a spectator scalar sector during a phase transition at inflation's end, with detailed analysis of particle production and relic abundance.

Findings

Dark matter abundance can be explained within a restricted parameter space.

Spectator particle decay into dark matter dominates the relic abundance.

Elastic self-scatterings effectively redistribute spectator particle momenta.

Abstract

We study whether a first-order phase transition at the end of inflation can generate the observed dark matter abundance through bubble collisions. The transition occurs in a spectator scalar sector with an inflaton-dependent effective potential, so that the nucleation rate grows during inflation and becomes significant only near its end. We identify the region of parameter space in which vacuum decay is dominated by the Coleman--De~Luccia channel, the Hawking--Moss transition remains subdominant, and the nucleated bubbles admit a consistent physical interpretation in an inflating background. Requiring also that the phase transition completes successfully, we then analyze particle production from bubble collisions. In the viable regime, elastic self-scatterings of the spectator particles can efficiently redistribute their momenta, while their decay into dark matter provides the dominant channel for transferring the spectator population to the dark sector. Other competing number-changing or sink processes remain inefficient compared with the Hubble expansion. The final relic abundance receives contributions from both direct production in bubble collisions and the subsequent decay of spectator field particles. We find that the observed dark matter abundance can be accommodated, within the order-of-magnitude accuracy of the collision-production treatment, in a restricted region of parameter space.