Hotspots around light primordial black holes cool faster in an expanding universe following T_plt ∝ t^{-11/15} and vanish completely in finite time, unlike everlasting hotspots in flat spacetime.
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Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.
Memory-burden backreaction deforms the Hawking spectrum to suppress its high-energy tail, lowering total luminosity and neutrino flux by a factor set by a single suppression parameter and thereby relaxing IceCube bounds on primordial black hole dark matter.
Skyrmion black holes show modified photon spheres, shadows, and sparser Hawking radiation due to the Skyrme coupling strength and background parameters.
The perfect fluid dark matter parameter dominates the effects on shadow size, quasinormal frequencies, and energy emission rates, while the Euler-Heisenberg correction remains subleading in the explored regime.
citing papers explorer
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Primordial Black Hole Hotspots Beyond Flat Spacetime
Hotspots around light primordial black holes cool faster in an expanding universe following T_plt ∝ t^{-11/15} and vanish completely in finite time, unlike everlasting hotspots in flat spacetime.
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The Magnetic Origin of Primordial Black Holes: Ultralight PBHs and Secondary GWs
Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.
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Memory-Burden Suppression of Hawking Radiation and Neutrino Constraints on Primordial Black Holes
Memory-burden backreaction deforms the Hawking spectrum to suppress its high-energy tail, lowering total luminosity and neutrino flux by a factor set by a single suppression parameter and thereby relaxing IceCube bounds on primordial black hole dark matter.
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Shadow, Sparsity of Radiation and Energy Emission Rate in Skyrmion Black Holes
Skyrmion black holes show modified photon spheres, shadows, and sparser Hawking radiation due to the Skyrme coupling strength and background parameters.
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Shadow, Quasinormal Modes, Sparsity, and Energy Emission Rate of Euler-Heisenberg Black Hole Surrounded by Perfect Fluid Dark Matter
The perfect fluid dark matter parameter dominates the effects on shadow size, quasinormal frequencies, and energy emission rates, while the Euler-Heisenberg correction remains subleading in the explored regime.