Structure and evolution of irradiated accretion disks. I - Static thermal equilibrium structure. II - Dynamical evolution of a thermally unstable torus

Details Structure and evolution of irradiated accretion disks. I - Static thermal equilibrium structure. II - Dynamical evolution of a thermally unstable torus Structure and evolution of irradiated accretion disks. I - Static thermal equilibrium structure. II - Dynamical evolution of a thermally unstable torus

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...359..164t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 359, Aug. 10, 1990, p. 164-185.

Astronomy and Astrophysics

Astronomy

56

Accretion Disks, Dwarf Stars, Stellar Evolution, Stellar Structure, X Ray Binaries, Black Holes (Astronomy), Boundary Conditions, Light Curve, Mass Transfer, Neutron Stars, Thermal Stability

Scientific paper

The thermal equilibrum structure and dynamical behavior of externally irradiated accretion disks are investigated. For radiative disks only the surface layer is heated, while for convective disks the heat penetrates deeply into the disk. For sufficiently strong radiation and given irradiation flux F(irr), the disk is completely stabilized against thermal instabilities of the sort invoked to explain dwarf novae. For moderately strong irradiation there is still an unstable branch in the thermal equilibrium curve. In typical soft X-ray transients, the disk is unstable against the dwarf-nova type instability. Fixed F(irr) on accretion disk annuli reduces the amplitude and the quiescent times and increases the outburst duration of the resultant light curves. Varying F(irr) in proportion to the mass accretion rate at the disks's inner edge results in light curves with a plateau in the decay from outbursts. In the case when irradiation is suddenly switched on, a temperature inversion results which leads to the formation of an accretion corona.

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