A warped 5D geometry with hidden-sector accretion produces growing Schwarzschild/Vaidya black-hole seeds on our brane via a common horizon intersection.
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Non-equilibrium relativistic SIDM halo collapse produces seed black holes of mass ~3e-8 of the halo mass at apparent horizon formation.
Axion dark matter decay injects 1-13.6 eV photons that suppress H2, enabling atomic cooling halos and direct collapse black hole seeds for axion masses 24.5-26.5 eV and couplings down to 4e-12/GeV.
GW231123's masses and high spins are consistent with primordial black holes that accreted mass and angular momentum in the early universe within the standard PBH framework.
A source 660 million years after the Big Bang is interpreted as a black hole star with a dust-free dense gas atmosphere, implying Little Red Dots have black hole masses overestimated by orders of magnitude.
Generalization of scalar-fermion Yukawa systems in constant-EOS cosmologies identifies scaling regime with constant energy density ratio from approximate scale invariance and asymptotic regime recovering bare mass.
New ALMA [C II] and FIR data on PSO J083+11 at z=6.34 reveal ordered rotation, typical star-forming ratios, and no outflow signatures in either galaxy, interpreted as a pre-AGN-feedback accretion phase.
Regular primordial black holes can evaporate completely like singular ones and yield the observed dark matter density under modified cosmological constraints.
MCMC comparison of projected PBH correlation functions with z≈6 quasar angular auto-correlation data yields posterior constraints f_PBH∼10^{-3}, m_PBH∼10^{12}M_⊙ for Poisson models and ξ_eff≃2.1, r_cl≃76 Mpc for clustered models.
citing papers explorer
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Hidden-sector accretion and warped black-string seeds for high-redshift supermassive black holes
A warped 5D geometry with hidden-sector accretion produces growing Schwarzschild/Vaidya black-hole seeds on our brane via a common horizon intersection.
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Non-Equilibrium Relativistic Core Collapse of Self-Interacting Dark Matter Halos -- Limits On Seed Black Hole Mass
Non-equilibrium relativistic SIDM halo collapse produces seed black holes of mass ~3e-8 of the halo mass at apparent horizon formation.
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Direct Collapse Black Hole Candidates from Decaying Dark Matter
Axion dark matter decay injects 1-13.6 eV photons that suppress H2, enabling atomic cooling halos and direct collapse black hole seeds for axion masses 24.5-26.5 eV and couplings down to 4e-12/GeV.
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GW231123: A Possible Primordial Black Hole Origin
GW231123's masses and high spins are consistent with primordial black holes that accreted mass and angular momentum in the early universe within the standard PBH framework.
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A "Black Hole Star" Reveals the Remarkable Gas-Enshrouded Hearts of the Little Red Dots
A source 660 million years after the Big Bang is interpreted as a black hole star with a dust-free dense gas atmosphere, implying Little Red Dots have black hole masses overestimated by orders of magnitude.
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The cosmology of long range Yukawa interactions in general backgrounds
Generalization of scalar-fermion Yukawa systems in constant-EOS cosmologies identifies scaling regime with constant energy density ratio from approximate scale invariance and asymptotic regime recovering bare mass.
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A Quasar--Companion System Without AGN Outflow at $z \sim 6$: The Case of PSO J083+11
New ALMA [C II] and FIR data on PSO J083+11 at z=6.34 reveal ordered rotation, typical star-forming ratios, and no outflow signatures in either galaxy, interpreted as a pre-AGN-feedback accretion phase.
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Dark matter production from evaporation of regular primordial black holes
Regular primordial black holes can evaporate completely like singular ones and yield the observed dark matter density under modified cosmological constraints.
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Constraining supermassive primordial black hole clustering with the angular auto-correlation of $z\simeq 6$ quasars
MCMC comparison of projected PBH correlation functions with z≈6 quasar angular auto-correlation data yields posterior constraints f_PBH∼10^{-3}, m_PBH∼10^{12}M_⊙ for Poisson models and ξ_eff≃2.1, r_cl≃76 Mpc for clustered models.