Non-equilibrium relativistic SIDM halo collapse produces seed black holes of mass ~3e-8 of the halo mass at apparent horizon formation.
Title resolution pending
7 Pith papers cite this work. Polarity classification is still indexing.
7
Pith papers citing it
citation-role summary
background 3
citation-polarity summary
roles
background 3polarities
background 3representative citing papers
Monte Carlo solutions of the Smoluchowski equation for PBH clusters yield finite runaway timescales and evolving mass distributions that form high-redshift SMBHs, shortened further by mass segregation.
A relativistic self-interacting dark-matter fluid near a critical sound speed gives a universal Bondi accretion rate that can grow 10-solar-mass seed black holes into 10^9–10^10 solar-mass supermassive black holes by z≈7.
SIDM core-collapse simulations produce a dense central core matching the lensing perturber, while CDM requires an IMBH with extreme tidal mass loss whose realism is left open.
MW-mass SIDM halos bypass core formation and enter immediate core collapse due to baryonic preconditioning, allowing the compact stellar disk and bulge to survive close pericenter passages while the diffuse halo is more easily disrupted.
1D hydrodynamic simulations find that SIDM heat transport competes with gravity to regulate black hole accretion, enabling rapid growth in SIS profiles up to 10,000 solar masses from a 100 solar mass seed in 2 Myr.
Baryonic feedback mildly delays but does not stall gravothermal collapse in high-concentration SIDM halos and allows resumption in median-concentration cases, yielding feedback-history-dependent central densities.
citing papers explorer
-
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.
-
Smoluchowski Coagulation Equation and the Evolution of Primordial Black Hole Clusters
Monte Carlo solutions of the Smoluchowski equation for PBH clusters yield finite runaway timescales and evolving mass distributions that form high-redshift SMBHs, shortened further by mass segregation.
-
A Unified Dark-Matter--Driven Relativistic Bondi Route to Black-Hole Growth from Stellar to Supermassive Scales
A relativistic self-interacting dark-matter fluid near a critical sound speed gives a universal Bondi accretion rate that can grow 10-solar-mass seed black holes into 10^9–10^10 solar-mass supermassive black holes by z≈7.
-
SIDM and CDM interpretations of the million-solar-mass lensing perturber JVAS B1938+666-$\mathcal{V}$
SIDM core-collapse simulations produce a dense central core matching the lensing perturber, while CDM requires an IMBH with extreme tidal mass loss whose realism is left open.
-
Bypassed Core Formation in Milky Way-Mass SIDM Halos: Implications for the Local Group Past-Pericenter Scenario
MW-mass SIDM halos bypass core formation and enter immediate core collapse due to baryonic preconditioning, allowing the compact stellar disk and bulge to survive close pericenter passages while the diffuse halo is more easily disrupted.
-
Spherically Symmetric Fluid Simulations of Black Hole Accretion in Self-Interacting Dark Matter Halos
1D hydrodynamic simulations find that SIDM heat transport competes with gravity to regulate black hole accretion, enabling rapid growth in SIS profiles up to 10,000 solar masses from a 100 solar mass seed in 2 Myr.
-
Gravothermal Collapse: Robust Against Baryonic Feedback
Baryonic feedback mildly delays but does not stall gravothermal collapse in high-concentration SIDM halos and allows resumption in median-concentration cases, yielding feedback-history-dependent central densities.