Radiation hydrodynamics of the boundary layer in accretion disks. II - Optically thick models

Details Radiation hydrodynamics of the boundary layer in accretion disks. II - Optically thick models Radiation hydrodynamics of the boundary layer in accretion disks. II - Optically thick models

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...222..141k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 222, no. 1-2, Sept. 1989, p. 141-149.

Statistics

Computation

53

Accretion Disks, Cataclysmic Variables, Computational Astrophysics, Hydrodynamics, Stellar Models, White Dwarf Stars, Angular Velocity, Boundary Layers, Radiation Distribution, Stellar Coronas, Stellar Rotation

Scientific paper

This paper presents the results of two-dimensional numerical radiation hydrodynamical calculations on the structure of the optically thick boundary layer between the white dwarf and the accretion disk in Cataclysmic Variables. The boundary layer forms an equatorial belt around the white dwarf with a radial extent of less than about 0.005 R(WD) and a vertical extent of about 7.5 deg. The major part of the dissipated energy is liberated outside the boundary layer where the temperature also peaks. The maximum temperature depends on the rotation rate of the white dwarf. In the vicinity of the boundary layer the gas in the disk has a strongly supersonic radial infall velocity. Around the star and above the disk, a hot corona is formed. Observationally, the optically thick boundary layer influences mainly the soft X-ray and the far-UV region of the spectrum and, at higher inclinations, also the UV.

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