Black holes and gravitational waves from slow phase transitions

2024/02/06 by Marek Lewicki, Lewicki, Marek, Piotr Toczek +3 · 11 citations
Physics and Astronomy · #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Physics - Phenomenology (hep-ph) #Pulsars and Gravitational Waves Research #Relativity and Gravitational Theory

paper · pdf · doi:10.48550/arxiv.2402.04158

openalex publication_date 2024/02/06 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

Slow first-order phase transitions generate large inhomogeneities that can lead to the formation of primordial black holes (PBHs). We show that the gravitational wave (GW) spectrum then consists of a primary component sourced by bubble collisions and a secondary one induced by large perturbations. The latter gives the dominant peak if β/H₀ < 12, impacting, in particular, the interpretation of the recent PTA data. The GW signal associated with a particular PBH population is stronger than in typical scenarios because of a negative non-Gaussianity of the perturbations and it has a distinguishable shape with two peaks.

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• The curvature perturbations and induced gravitational waves induced by the first-order phase transition during reheating
• Boiling After the Dust Settles: Constraining First-Order Phase Transitions During Dark Energy Domination
• Implications for Pulsar Timing Arrays of Sub-solar Black Hole Detections: From LVK to Einstein Telescope and Cosmic Explorer
• Induced phase transitions and spontaneous symmetry breaking based on the renormalized Ginzburg-Landau theory
• Significance of soft-scale breaking on primordial black hole production in Coleman-Weinberg type supercooling-phase transition
• Acoustically driven dark matter freeze-out
• Can asteroid-mass PBHDM be compatible with catalyzed phase transition interpretation of PTA?
• Acoustic gravitational waves beyond leading order in bubble over Hubble radius

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