Thick accretion disks with super-Eddington luminosities

Journal Article · Mon Dec 01 04:00:00 EST 1980 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/158512· OSTI ID:6525321

Abramowicz, M A; Calvani, M; Nobili, L

We describe a Newtonian version of the theory of thick accretion disks orbiting black holes. In view of the present inadequate knowledge of microscopic viscosity process, this theory adopts a macroscopic approach. All the uncertainties are absorbed in currently arbitrary functions lambda(xi) and f(xi) which describe the (non-Keplerian) angular momentum along the disk, and the outgoing radiation flux in units of the critical flux. Assuming surface distributions of angular momentum and radiation flux, one can construct a model of a thick, non-Keplerian accretion disk with no knowledge of the viscosity mechanism. Thick accretion disks can have luminosities 100 times above the Eddington limit. We study the self-consistency constraints for the theory of thick accretion disks with super-Eddington luminosities.

• Research Organization: Center for Relativity, Department of Physics, The University of Texas at Austin
• OSTI ID: 6525321
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 242:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR MOMENTUM
BLACK HOLES
COSMIC RADIO SOURCES
EDDINGTON THEORY
EQUILIBRIUM
GALAXY NUCLEI
GRAVITATION
LUMINOSITY
MATHEMATICAL MODELS
OPTICAL PROPERTIES
ORBITS
PHYSICAL PROPERTIES
QUASARS
RADIATION FLUX
STAR ACCRETION
STAR EVOLUTION
STAR MODELS