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ROSAT observations of non-magnetic CVs

Published online by Cambridge University Press:  12 April 2016

A. van Teeseling ,
F. Verbunt  and
K. Beuermann
A. van Teeseling
Affiliation:
Universitäts-Sternwarte Göttingen, Germany
F. Verbunt
Affiliation:
Astronomical Institute, Utrecht, The Netherlands
K. Beuermann
Affiliation:
Universitäts-Sternwarte Göttingen, Germany

Extract

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In non-magnetic cataclysmic variables the accreted matter forms an accretion disk around the white dwarf. In the boundary layer between the white dwarf and the accretion disk the accreted matter decelerates from Keplerian velocities to the rotation velocity of the white dwarf. If the accretion rate is high the boundary layer would be optically thick and cool (T ~ 105K), and if the accretion rate is low the boundary layer would be optically thin and hot (T ~ 108K) (Pringle & Savonije 1979).

There are several observational problems with this simple picture: a soft X-ray component could only be detected so far in 5 dwarf novae in outburst and not in any nova-like variable. Also in high-accretion-rate systems there is a hot optically thin X-ray source, which has, however, an X-ray luminosity which is much less than the UV luminosity of the system (van Teeseling & Verbunt 1994). Finally, there is evidence for orbital modulation in the X-rays from some systems (e.g. van Teeseling et al. 1995).

Type
Space Observations
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 273 - 276
Copyright
Copyright © Kluwer 1996

References

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