The Accretion Disk and White Dwarf during the Quiescence of the Dwarf Novae VW Vulpeculae and χ Leonis

Details The Accretion Disk and White Dwarf during the Quiescence of the Dwarf Novae VW Vulpeculae and χ Leonis The Accretion Disk and White Dwarf during the Quiescence of the Dwarf Novae VW Vulpeculae and χ Leonis

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001pasp..113..970h&link_type=abstract

The Publications of the Astronomical Society of the Pacific, Volume 113, Issue 786, pp. 970-973.

Astronomy and Astrophysics

Astronomy

5

Stars: Novae, Cataclysmic Variables, Stars: Individual (Vw Vulpeculae), Stars: Individual (Χ Leonis)

Scientific paper

We have carried out an International Ultraviolet Explorer archival comparative study of the two U Geminorum type dwarf novae VW Vulpeculae and χ Leonis. The spectrum of χ Leo does not show any C IV, a feature normally seen in the vast majority of other dwarf novae. For VW Vul, a single-temperature high-gravity photosphere does not produce a consistent fit. The best-fit accretion disk model corresponds to Mwd=0.55 Msolar, i=41deg, and M=10-9 Msolar yr-1. For χ Leo, we find that a white dwarf model with Teff=33,000 K gives the best fit to the far-UV spectrum. However, a model accretion disk with parameters M=0.80 Msolar, i=60deg, and M=10-10 Msolar yr-1 also gives a satisfactory fit to the far-UV continuum. However, the accretion rate derived for VW Vul is within a factor of 3 of the critical value, while the accretion rate of χ Leo is within a factor of 60 of the critical rate. If we have identified the accreting white dwarf in χ Leo, then it strengthens the overall conclusion that the white dwarfs in cataclysmic variables above the period gap appear to be a factor of 1.5-2 times hotter than the accreting white dwarfs in dwarf novae below the period gap.

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