A Far Ultraviolet Study of the Hot White Dwarf in the Dwarf Nova WW Ceti

Details A Far Ultraviolet Study of the Hot White Dwarf in the Dwarf Nova WW Ceti A Far Ultraviolet Study of the Hot White Dwarf in the Dwarf Nova WW Ceti

2006-02-06

arxiv.org/abs/astro-ph/0602120v1

Astron.J.131:2634-2642,2006

Astronomy and Astrophysics

Astrophysics

25 pages, 3 tables, 8 figures (including 2 color ones), final version

Scientific paper

10.1086/501523

We present a synthetic spectral analysis of IUE archival and FUSE FUV spectra of the peculiar dwarf nova WW Ceti. During the quiescence of WW Ceti, a white dwarf with Twd=26,000K can account for the FUV flux and yields the proper distance. However, the best agreement with the observations is provided by a two-temperature white dwarf model with a cooler white dwarf at Twd=25,000K providing 75% of the FUV flux and a hotter region (accretion belt or optically thick disk ring) with T=40,000K contributing 25% of the flux for the proper distance. We find from the FUSE spectrum that the white dwarf is rotating with a projected rotational velocity V sin{i} = 600 km/s. Our temperature results provide an additional data point in the distribution of Twd versus orbital period above the CV period gap where few Twds are available.

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