An X-ray corona in SS Cygni?

Details An X-ray corona in SS Cygni? An X-ray corona in SS Cygni?

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985natur.313..290k&link_type=abstract

Nature (ISSN 0028-0836), vol. 313, Jan. 24, 1985, p. 290, 291.

Astronomy and Astrophysics

Astronomy

10

Dwarf Novae, Spaceborne Astronomy, Stellar Coronas, X Ray Sources, Bremsstrahlung, Cross Correlation, Exosat Satellite, Stellar Luminosity

Scientific paper

Some results from an about 7.5 hr EXOSAT observation of the dwarf nova SS Cygni in its quiescent state are presented. These results confirm many predictions of a recent model for the X-ray emission from nonmagnetic cataclysmic variables which suggests that most of the observed hard X-ray flux originates in a radiatively-cooling quasi-hydrostatic corona surrounding the white dwarf as it accretes from its companion. In particular, the results show that the X-ray luminosity and bremsstrahlung temperature obey the predicted relationship. They also suggest that the emitting region covers an appreciable fraction of the white dwarf's surface and that transport processes into the white dwarf cause most of the luminosity to emerge at soft X-ray/extreme ultraviolet wavelengths.

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