REVIEW 6 cited by
Collapse of Primordial Gas Clouds and the Formation of Quasar Black Holes
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Collapse of Primordial Gas Clouds and the Formation of Quasar Black Holes
read the original abstract
The formation of quasar black holes during the hydrodynamic collapse of protogalactic gas clouds is discussed. The dissipational collapse and long- term dynamical evolution of these systems is analysed using three-dimensional numerical simulations. The calculations focus on the final collapse stages of the inner baryonic component and therefore ignore the presence of dark matter. Two types of initial conditions are considered: uniformly rotating spherical clouds, and irrotational ellipsoidal clouds. In both cases the clouds are initially cold, homogeneous, and not far from rotational support ($T/|W| \approx 0.1$). Although the details of the dynamical evolution depend sensitively on the initial conditions, the qualitative features of the final configurations do not. Most of the gas is found to fragment into small dense clumps, that eventually make up a spheroidal component resembling a galactic bulge. About 5\% of the initial mass remains in the form of a smooth disk of gas supported by rotation in the gravitational potential well of the outer spheroid. If a central seed black hole of mass $\gsim10^6M_\odot$ forms, it can grow by steady accretion from the disk and reach a typical quasar black hole mass $\sim10^8M_\odot$ in less than $5\times 10^8\,$yr. In the absence of a sufficiently massive seed, dynamical instabilities in a strongly self- gravitating inner region of the disk will inhibit steady accretion of gas and may prevent the immediate formation of a quasar.
Forward citations
Cited by 6 Pith papers
-
Too shy to spin? Cosmic wallflowers as proto-globular clusters
Simulation study proposes that weakly rotating, gas-rich cosmic wallflowers at high redshift are natural proto-globular cluster candidates based on kinematics and densities.
-
TDEs on FIRE: Illuminating the Cosmic Evolution of Tidal Disruption Rates
FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.
-
A quasi-star is born: formation and evolution of accreting quasi-stars as a pathway to Little Red Dots at non-zero metallicity
Rapidly accreting supermassive stars that collapse to black holes can form quasi-stars whose light matches the Little Red Dots seen by JWST, independent of metallicity.
-
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.
-
Too shy to spin? Cosmic wallflowers as proto-globular clusters
Star clusters forming in cosmic filaments at z≈7.6 are systematically slow rotators, and a gas-rich subset overlaps the kinematic and density locus of Milky Way globular clusters, making them plausible proto-globular ...
-
Ultraviolet diversity of Little Red Dots as a probe for direct-collapse black hole ages
Cosmological hydrodynamical simulations predict that UV diversity in Little Red Dots encodes direct-collapse black hole ages via a rapid transition from BH- to stellar-dominated emission after ~30 Myr.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.