Accounting for the minimal mass spread of primordial black holes from gravitational collapse suppresses the Poltergeist GW background to the level of generic scalar-induced signals and reopens ultra-light PBH parameter space.
Primordial black hole formation by vacuum bubbles. Part II
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DBI domain walls stay shock-free in the hyperbolic regime across 2D flat space and extended physical setups, with caustics forming only upon loss of hyperbolicity and exhibiting cusp profiles.
Tensor perturbations from first-order phase transitions and domain wall annihilation induce curvature fluctuations at second order that form primordial black holes, allowing asteroid-mass PBHs to comprise all dark matter for specific parameter ranges with associated gravitational wave peaks in LISA,
Sound shell collisions from Hubble-scale primordial density perturbations generate a stochastic GW background whose peak frequency and amplitude scale with the Hubble horizon and shell abundance.
citing papers explorer
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Gravitational Waves from Black Hole Reheating: The Scalar-Induced Component
Accounting for the minimal mass spread of primordial black holes from gravitational collapse suppresses the Poltergeist GW background to the level of generic scalar-induced signals and reopens ultra-light PBH parameter space.
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Hard to shock DBI: wave propagation on planar domain walls
DBI domain walls stay shock-free in the hyperbolic regime across 2D flat space and extended physical setups, with caustics forming only upon loss of hyperbolicity and exhibiting cusp profiles.
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Primordial Black Hole from Tensor-induced Density Fluctuation: First-order Phase Transitions and Domain Walls
Tensor perturbations from first-order phase transitions and domain wall annihilation induce curvature fluctuations at second order that form primordial black holes, allowing asteroid-mass PBHs to comprise all dark matter for specific parameter ranges with associated gravitational wave peaks in LISA,
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Relic gravitational waves from primordial gravitational collapses
Sound shell collisions from Hubble-scale primordial density perturbations generate a stochastic GW background whose peak frequency and amplitude scale with the Hubble horizon and shell abundance.