Volume 397, Number 3, January III 2003
|Page(s)||961 - 967|
|Section||Stellar structure and evolution|
|Published online||21 January 2003|
A model of the dwarf nova WX Cet
Adam Mickiewicz University Observatory, ul. Sloneczna 36, 60-286 Poznań, Poland
2 Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland e-mail: email@example.com
Corresponding author: P. Rogoziecki, firstname.lastname@example.org
Accepted: 22 October 2002
We analyse time-resolved spectroscopy of WX Cet, a dwarf nova of the WZ Sge class, by means of a dynamical model based on the measured K1 and using the superhump period excess ϵ to constrain the mass ratio q of this CB. From time resolved spectroscopy of Thorstensen et al. we determine orbital amplitude K1 and separation of the disk emission lines as well as the S-wave amplitude As and relative phase α of the hot spot. Our dynamical analysis, following Smak's inclination independent solution for WZ Sge, yields rather high q, hardly compatible with the superhump resonance condition within the accretion disc. Rejecting K1 as affected by tidal and/or stream effects, we follow Patterson and determine from relation based on superhump dynamics. In this way we obtain likely masses of the components and . From this result we argue that despite similarities to WZ Sge, WX Cet with its relatively massive secondary represents an earlier stage of mass transfer in a cataclysmic binary than WZ Sge.
Key words: stars: novae, cataclysmic variables / stars: dwarf novae / stars individual: WX Cet / stars individual: WZ Sge / accretion, accretion disks
© ESO, 2003
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