Correlated signals of first-order phase transitions and primordial black hole evaporation

Marfatia, Danny; Tseng, Po-Yan

doi:10.48550/arxiv.2112.14588

Cited by 3 publications

(3 citation statements)

References 41 publications

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“…Phase transition GWs. PBHs can form during a first-order phase transition via trapping fermions in the false vacuum [486][487][488][489][490], bubble collisions [491,492] or postponed vacuum decay [493,494]. In such scenarios, there could be correlated signals between PBHs (e.g.…”

Section: Bh Mergers At High Redshift the Third Generation Of Gw Detec...mentioning

confidence: 99%

Detection of early-universe gravitational-wave signatures and fundamental physics

et al. 2022

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Detection of a gravitational-wave signal of non-astrophysical origin would be a landmark discovery, potentially providing a significant clue to some of our most basic, big-picture scientific questions about the Universe. In this white paper, we survey the leading early-Universe mechanisms that may produce a detectable signal—including inflation, phase transitions, topological defects, as well as primordial black holes—and highlight the connections to fundamental physics. We review the complementarity with collider searches for new physics, and multimessenger probes of the large-scale structure of the Universe.

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Section: Bh Mergers At High Redshift the Third Generation Of Gw Detec...mentioning

confidence: 99%

Detection of early-universe gravitational-wave signatures and fundamental physics

et al. 2022

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“…Cosmic first-order phase transitions (FOPTs) provide a favorable environment for PBH formation: the Universe transitions from a higher energy false vacuum to a lower energy true vacuum via tunneling, resulting in the true vacuum bubbles nucleate and expand in the false vacuum background. This may lead to the formation of PBHs, if the bubble collisions compress a large amount of energy into a small volume [5][6][7], or if some false vacuum remnants form significant overdensities via delayed vacuum decay or trapping fermions [29][30][31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47]. While FOPTs might be generic during the thermal history of the Universe [48], the formation of PBHs during such transitions is highly nontrivial.…”

Section: Introductionmentioning

confidence: 99%

Primordial black holes from slow phase transitions: a model-building perspective

Kanemura,

Tanaka,

Xie

2024

J. High Energ. Phys.

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We investigate the formation of primordial black holes (PBHs) through delayed vacuum decay during slow cosmic first-order phase transitions. Two specific models, the polynomial potential and the real singlet extension of the Standard Model, are used as illustrative examples. Our findings reveal that models with zero-temperature scalar potential barriers are conducive to the realization of this mechanism, as the phase transition duration is extended by the U-shaped Euclidean action. We find that the resulting PBH density is highly sensitive to the barrier height, with abundant PBH formation observed for sufficiently high barriers. Notably, the phase transition needs not to be ultra-supercooled (i.e. the parameter α ≫ 1), and the commonly used exponential nucleation approximation Γ(t) ~ eβt fails to capture the PBH formation dynamics in such models.

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“…Introduction.-One intriguing possibility for going beyond the standard model (BSM) of particle physics in the early Universe is the presence of the cosmological first-order phase transitions (FOPTs) [1][2][3]. Besides the stochastic gravitational wave backgrounds (SGWBs) [4][5][6][7], the production of primordial black holes is also a universal consequence of the cosmological FOPTs [8,9] (see also [10][11][12][13][14] for other specific mechanisms). The associated non-equilibrium nature during FOPT can also be used to explain the baryon asymmetry [15] and primordial magnetic fields [16].…”

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confidence: 99%

Hydrodynamic backreaction force of cosmological bubble expansion

Wang,

Yuwen

2022

Preprint

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As a promising probe for the new physics beyond the standard model of particle physics in the early Universe, the predictions for the stochastic gravitational wave background from a cosmological firstorder phase transition heavily rely on the bubble wall velocity determined by the bubble expansion dynamics. The bubble expansion dynamics is governed by the competition between the driving force from the effective potential difference and the backreaction force from a sum of the thermal and friction forces induced by the temperature jumping and out-of-equilibrium effects across the bubble wall, respectively. Recently, a thermodynamic evaluation for the difference ∆[(γ 2 − 1)w] in the vicinity of the bubble wall is proposed to account for this backreaction force in a local thermal equilibrium from the enthalpy w and the Lorentz factor γ ≡ (1 − v2 ) −1/2 of the wall-frame fluid velocity v. However, this proposal has neglected the hydrodynamic contribution from the sound shell with a non-vanishing fluid velocity profile. In this paper, we propose a complete hydrodynamic evaluation on the backreaction force for a non-runaway bubble expansion, whose wall contribution exactly matches the previous thermodynamic evaluation.

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Correlated signals of first-order phase transitions and primordial black hole evaporation

Cited by 3 publications

References 41 publications

Detection of early-universe gravitational-wave signatures and fundamental physics

Detection of early-universe gravitational-wave signatures and fundamental physics

Primordial black holes from slow phase transitions: a model-building perspective

Hydrodynamic backreaction force of cosmological bubble expansion

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