On the X-ray emitting boundary layer of the dwarf nova VW Hydri

Details On the X-ray emitting boundary layer of the dwarf nova VW Hydri On the X-ray emitting boundary layer of the dwarf nova VW Hydri

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...372..659m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 372, May 10, 1991, p. 659-663.

Astronomy and Astrophysics

Astrophysics

34

Dwarf Novae, Stellar Spectrophotometry, Ultraviolet Photometry, X Ray Sources, Accretion Disks, Exosat Satellite, Hydrogen Atoms, Stellar Luminosity, Stellar Temperature

Scientific paper

The temperature and luminosity of the boundary layer of VW Hyi are constrained to kT(BL) of about 10.5 eV, and L(BL) of about 6 x 10 to the 32nd (d/65 pc)squared ergs/sec. This is based on Voyager far- and extreme-ultraviolet spectrophotometry and a measurement of the column density of neutral hydrogen, combined with Exosat LE filter observations. Results are compared with the accretion-disk luminosity found by Polidan et al. (1990) using concurrent optical, IUE, and Voyager spectrophotometric observations. The value of zeta is found to be about 0.04, although theoretical predictions show comparable luminosities at the boundary layer and the accretion disk - zeta is identical to L(BL)/L(disk), which is about 1 - unless the white dwarf rotates very rapidly. Severe contamination of filter observations due to light from the inner accretion disk is also found. This contamination had previously been understood as a result of the luminous ultrasoft boundary layer.

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