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Title:
Observations of the Magnetic Cataclysmic Variable VV Puppis with the Far Ultraviolet Spectroscopic Explorer
Authors:
Hoard, D. W.; Szkody, Paula; Ishioka, Ryoko; Ferrario, L.; Gänsicke, B. T.; Schmidt, Gary D.; Kato, Taichi; Uemura, Makoto
Affiliation:
AA(Department of Astronomy, University of Washington, Box 351580, Seattle WA 98195-1580 , ), AB(Department of Astronomy, University of Washington, Box 351580, Seattle WA 98195-1580 , ), AC(Department of Astronomy, Faculty of Science, Kyoto University, Sakyou-ku, Kyoto, 606-8502, Japan; ), AD(Department of Mathematics, Australian National University, Canberra, ACT 0200, Australia; ), AE(Department of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ, UK; ), AF(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065 ), AG(Department of Astronomy, Faculty of Science, Kyoto University, Sakyou-ku, Kyoto, 606-8502, Japan; , ), AH(Department of Astronomy, Faculty of Science, Kyoto University, Sakyou-ku, Kyoto, 606-8502, Japan; , )
Publication:
The Astronomical Journal, Volume 124, Issue 4, pp. 2238-2244. (AJ Homepage)
Publication Date:
10/2002
Origin:
UCP
AJ Keywords:
Stars: Circumstellar Matter, Stars: Novae, Cataclysmic Variables, Stars: Individual: Constellation Name: VV Puppis, Stars: Magnetic Fields, Ultraviolet Emission
DOI:
10.1086/342547
Bibliographic Code:
2002AJ....124.2238H

Abstract

We present the first far-ultraviolet (FUV) observations of the magnetic cataclysmic variable VV Puppis, obtained with the Far Ultraviolet Spectroscopic Explorer satellite. In addition, we have obtained simultaneous ground-based optical photometric observations of VV Pup during part of the FUV observation. The shapes of the FUV and optical light curves are consistent with each other and with those of past observations at optical, extreme-ultraviolet, and X-ray wavelengths. Time-resolved FUV spectra during the portion of VV Pup's orbit when the accreting magnetic pole of the white dwarf can be seen show an increasing continuum level as the accretion spot becomes more directly visible. The most prominent features in the spectrum are the O VI λλ1031.9, 1037.6 emission lines. We interpret the shape and velocity shift of these lines in the context of an origin in the accretion funnel near the white dwarf surface. A blackbody function with Tbb>~90,000 K provides an adequate fit to the FUV spectral energy distribution of VV Pup. Based on observations with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer. FUSE is operated for NASA by Johns Hopkins University under NASA contract NAS 5-32985.
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