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Radiative Winds from Accretion Disks in CVS

Published online by Cambridge University Press:  25 May 2016

M. Hachiya ,
Y. Tajima  and
J. Fukue
M. Hachiya
Affiliation:
Astronomical Institute, Osaka Kyoiku University, Asahigaoka, Kashiwara, Osaka 582, Japan
Y. Tajima
Affiliation:
Astronomical Institute, Osaka Kyoiku University, Asahigaoka, Kashiwara, Osaka 582, Japan
J. Fukue
Affiliation:
Astronomical Institute, Osaka Kyoiku University, Asahigaoka, Kashiwara, Osaka 582, Japan

Extract

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P Cyg profiles observed in CVs strongly suggest the existence of accretion disk winds in CVs. Recently, X-ray observations revealed bipolar outflows in supersoft X-ray sources. The wind velocity measured in these observations is about 3000-5000 km s−1, which is of the order of the escape velocity of white dwarfs. Hence, it is supposed that the winds would originate from the inner disk and/or the boundary layers between the disk and white dwarf. We examine radiatively-acclerated accretion-disk winds, and found that the terminal speed of the wind emanated from the inner region becomes ~ 0.6GM/r in, where M is the white dwarf mass and r in the inner radius of the disk.

Information

Type
Session 3: Diagnostics of High Gravity Objects with X- and Gamma Rays
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 348 - 349
Copyright
Copyright © Kluwer 1998 

References

Tajima, Y., Fukue, J. 1996, PASJ 48, 529 Google Scholar
Tajima, Y., Fukue, J. 1997, in this volume Google Scholar