A model of the dwarf nova WX Cet

¹ Adam Mickiewicz University Observatory, ul. Sloneczna 36, 60-286 Poznań, Poland
² Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland e-mail: alex@camk.edu.pl

Corresponding author: P. Rogoziecki, progoz@moon.astro.amu.edu.pl

Received: 15 April 2002
Accepted: 22 October 2002

Abstract

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 A_s 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.