Physical properties of thick supercritical accretion disks

Details Physical properties of thick supercritical accretion disks Physical properties of thick supercritical accretion disks

May 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...256..666w&link_type=abstract

Astrophysical Journal, Part 1, vol. 256, May 15, 1982, p. 666-680.

Astronomy and Astrophysics

Astronomy

29

Black Holes (Astronomy), Stellar Mass Accretion, Stellar Models, Supercritical Flow, Disks (Shapes), Galactic Nuclei, Luminosity, Polytropic Processes, Viscosity

Scientific paper

Models of thick, super-Eddington accretion disks around black holes proposed by Paczynski and Wiita (1980) are analyzed. The shape and ratio of disk luminosity to Eddington luminosity essentially depend on the inner radius of the disk and the form of the (non-Keplerian) angular momentum distribution, whereas the size and actual luminosity grow linearly with the mass of the black hole. Two approaches are used in estimating the central temperatures and densities of such disks for different polytropic indices. In the first, the surface temperature and density are found first with the help of a parameter describing the ratio of radiation pressure to gas pressure in the atmosphere of the disk. The interior parameters, among them average values for the viscosity, are then found. The other approach fixes the form of the viscosity via a modification of the 'alpha-disk' relations and then proceeds to yield values of central and surface variables. With both methods, physical constraints involving mechanical equilibrium, the total mass of the disk, and the onset of nuclear fusion are found to stringently limit self-consistent models.

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