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An X-ray corona in SS Cygni?

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Abstract

A recent model1 for the X-ray emission of non-magnetic cataclysmic variables 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. We present here some results from a ∼7.5-h EXOSAT observation of the dwarf nova SS Cygni in its quiescent state, which confirm many of the predictions of this model. In particular, they show that the X-ray luminosity, Lx, and bremsstrahlung temperature, T, obey the predicted relationship Lx α T3/2+2ε. The results further suggest that the emitting region covers an appreciable fraction f∼0.1–1 of the white dwarf's surface, and also 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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Authors and Affiliations

  1. Department of Astronomy, University of Leicester, Leicester, LE1 7RH, UK

    A. R. King

  2. X-Ray Astronomy Group, Physics Department, University of Leicester, Leicester, LE1 7RH, UK

    M. G. Watson

  3. Space Research Utrecht, 3527 HS, Utrecht, The Netherlands

    J. Heise

Authors
  1. A. R. King
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  2. M. G. Watson
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  3. J. Heise
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King, A., Watson, M. & Heise, J. An X-ray corona in SS Cygni?. Nature 313, 290–291 (1985). https://doi.org/10.1038/313290a0

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  • DOI: https://doi.org/10.1038/313290a0

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