Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...572..456s&link_type=abstract
The Astrophysical Journal, Volume 572, Issue 1, pp. 456-460.
Astronomy and Astrophysics
Astronomy
17
Accretion, Accretion Disks, Stars: Binaries: Close, Stars: Dwarf Novae, Stars: Individual: Constellation Name: Ru Pegasi, Stars: White Dwarfs
Scientific paper
We present the results of the first multicomponent synthetic spectral analysis of International Ultraviolet Explorer (IUE) archival spectra of the long-period dwarf nova RU Peg during quiescence. The best-fit, high-gravity, solar composition photosphere models yield Teff=50,000-53,000 K with scale factor distances of 250 pc. Optically thick accretion disk models imply accretion rates between 1×10-9 and 1×10-10Msolar yr-1 in order to match the steeply sloping far-UV continuum. However, the best-fit accretion disk models yield distances from 600 to 1300 pc, well beyond the estimated distance range of 130-300 pc. Using rough theoretical flux arguments and the distance estimates, we find better agreement between the observed far-UV luminosity and the predicted far-UV luminosity of a hot, massive, white dwarf model than with an accretion disk model. RU Peg appears to contain the hottest white dwarf yet found in a dwarf nova. We cannot rule out that the far-UV energy distribution is due to a multitemperature white dwarf with cooler, more slowly rotating higher latitudes and a rapidly spinning, hotter equatorial belt. We discuss implications of our analysis for theoretical predictions of the disk instability theory of dwarf nova outbursts. We discuss a comparison between RU Peg's white dwarf and the observed properties of other analyzed white dwarfs in dwarf novae.
Sion Edward M.
Urban Joel
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