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Accretion Disk Models
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Models of black hole accretion disks are reviewed, with an emphasis on the theory of hard X-ray production. The following models are considered: i) standard, ii) super-critical, iii) two-temperature, and iv) disk+corona. New developments have recently been made in hydrodynamical models of accretion and in phenomenological radiative models fitting the observed X-ray spectra. Attempts to unify the two approaches are only partly successful.
Forward citations
Cited by 4 Pith papers
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Turbulent electron-ion coronae around accreting black holes self-regulate into a two-temperature state that generates nonthermal ions and X-ray spectra consistent with observations including an MeV tail.
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Accretion Regimes of Neutrino-Cooled Flows onto Black Holes
A 1D relativistic disk model charts the accretion regimes of neutrino-cooled flows and predicts r-process outflows up to black hole masses of about 3000 solar masses.
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Very Massive, Rapidly Spinning Binary Black Hole Progenitors through Chemically Homogeneous Evolution -- The Case of GW231123
Chemically homogeneous evolution of very massive, low-metallicity binaries can naturally produce the high masses and spins inferred for GW231123, with spins limited by the critical rotation rate.
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BASS LIII: The Eddington Ratio as the Primary Regulator of the Fraction of X-ray Emission in Active Galactic Nuclei
In a hard-X-ray-selected sample of 236 nearby unobscured AGN, the 2-10 keV X-ray bolometric correction is primarily set by Eddington ratio, with the luminosity dependence vanishing below λEdd ≈ 0.01.
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