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

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dc.creatorGodon, P.
dc.creatorSeward, L.
dc.creatorSion, E. M.
dc.creatorSzkody, P.
dc.date2006-02-06
dc.date.accessioned2026-07-07T11:25:15Z
dc.date.available2026-07-07T11:25:15Z
dc.descriptionWe 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.
dc.description25 pages, 3 tables, 8 figures (including 2 color ones), final version
dc.identifierhttps://arxiv.org/abs/astro-ph/0602120
dc.identifierhttp://arxiv.org/abs/astro-ph/0602120
dc.identifierAstron.J.131:2634-2642,2006
dc.identifierdoi:10.1086/501523
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/195450
dc.subjectAstrophysics
dc.titleA Far Ultraviolet Study of the Hot White Dwarf in the Dwarf Nova WW Ceti
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