Accretion disc winds and coronae. II - Illumination by the central source

Details Accretion disc winds and coronae. II - Illumination by the central source Accretion disc winds and coronae. II - Illumination by the central source

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.241..839c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 241, Dec. 15, 1989, p. 839-847.

Astronomy and Astrophysics

Astronomy

25

Accretion Disks, Stellar Mass Ejection, Stellar Winds, X Ray Binaries, Illumination, Mass Transfer, Optical Thickness, Viscous Flow

Scientific paper

X-ray illumination by the central source intensifies the viscously driven mass loss from the surface of an accretion disk. The optical depth of the wind, and its constancy with central accretion rate, are in good agreement with observations of accretion disk corona sources in low-mass X-ray binaries. It is shown that more than half of the mass transfer rate may be blown away from the disk for typical binary parameters, in contrast to earlier work which suggested such an effect only for long orbital periods (greater than about 15 hr).

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