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

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 ±1000K can account for the FUV flux and yields the proper distance. However, the best agreement with the observations is provided by a twotemperature 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 V sin i = 600 ± 100km s. Our temperature results provide an additional data point in the distribution of WD Twd versus orbital period above the CV period gap where few WD Twds are available.