Detailed Calculation of Primordial Black Hole Formation During First-Order Cosmological Phase Transitions
arXiv:2110.00005 · doi:10.1103/PhysRevD.111.063544
Abstract
Primordial black holes could potentially form during a first-order cosmological phase transition due to a build-up of particles which are predominantly reflected from the advancing bubble walls. After discussing the general mechanism, we examine the criteria that need to be satisfied for a black hole to form. We then set out the Boltzmann equation that describes the evolution of the relevant phase space distribution function, carefully describing our treatment of the Liouville operator and the collision term. Assuming a spherical false vacuum pocket of sufficient size and a constant wall velocity, we find that black holes can form in a range of different scenarios.
33 pages, 6 figures; v2: improved discussion of phase transition dynamics; matches published version
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Cited by in corpus (11)
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- Explaining the PeV Neutrino Fluxes at KM3NeT and IceCube with Quasi-Extremal Primordial Black Holes
- What happens when supercooling is terminated by curvature flipping of the effective potential?
- Bubbles kick off primordial black holes to form more binaries
- Reheating after the Supercooled Phase Transitions with Radiative Symmetry Breaking
- Numerical simulations of primordial black hole formation via delayed first-order phase transitions
- Gravitational Waves and Primordial Black Holes produced by Dark Meta Stable Vacuum Decay
- The Dark Side of the Moon: Listening to Scalar-Induced Gravitational Waves