Disk accretion onto a black hole at subcritical luminosity

Details Disk accretion onto a black hole at subcritical luminosity Disk accretion onto a black hole at subcritical luminosity

Jul 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....59..111b&link_type=abstract

Astronomy and Astrophysics, vol. 59, no. 1, July 1977, p. 111-125.

Astronomy and Astrophysics

Astronomy

159

Black Holes (Astronomy), Radiation Pressure, Stellar Mass Accretion, Binary Stars, Gravitational Effects, Radiation Distribution, Stellar Luminosity, Stellar Magnetic Fields, Stellar Models, Stellar Structure, Temperature Effects

Scientific paper

The effect of radiation pressure on the structure of a black-hole accretion disk is investigated for the case where the total disk luminosity (L) approaches the Eddington limit (Lc). Particle motions in the disk radiation field and in the gravitational field of an associated nonrotating black hole are analyzed. The results obtained indicate that: (1) when L exceeds 0.1 Lc, nonlocal effects of the radiation field become significant, the disk is thicker than predicted by the standard model, and plasma heating by the radiative flux in optically thin regions is of importance; (2) for L of about 0.6 to 1.0 Lc, disk accretion is disrupted and mass outflow sets in; (3) the curl component of the radiation force generates electric currents and a magnetic field in the disk; (4) heat in the central disk region is vertically transported by convection, which produces an acoustic energy flux and heats the upper layers (or corona) of the disk; and (5) the hard X-ray flux from Cygnus X-1 may be explained by Comptonization in the hot disk corona of soft photons created in the lower disk layers.

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