Geometrically thin, hot accretion disks - Topology of the thermal equilibrium curves

Details Geometrically thin, hot accretion disks - Topology of the thermal equilibrium curves Geometrically thin, hot accretion disks - Topology of the thermal equilibrium curves

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...392..653k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 392, no. 2, June 20, 1992, p. 653-661. Research supported by U.S. National

Astronomy and Astrophysics

Astronomy

15

Accretion Disks, Black Holes (Astronomy), Bremsstrahlung, Compton Effect, Stellar Mass, Black Body Radiation, Radiation Pressure, Radiative Transfer, Thermodynamic Equilibrium

Scientific paper

All the possible thermal equilibrium states of geometrically thin alpha-disks around stellar-mass black holes are presented. A (vertically) one-zone disk model is employed and it is assumed that a main energy source is viscous heating of protons and that cooling is due to bremsstrahlung and Compton scattering. There exist various branches of the thermal equilibrium solution, depending on whether disks are effectively optically thick or thin, radiation pressure-dominated or gas pressure-dominated, composed of one-temperature plasmas or of two-temperature plasmas, and with high concentration of e(+)e(-) pairs or without pairs. The thermal equilibrium curves at high temperatures (greater than or approximately equal to 10 exp 8 K) are substantially modified by the presence of e(+)e(-) pairs. The thermal stability of these branches are examined.

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