2003A&A...397..961R

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 2V_d 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 q=0.085 from q-ε relation based on superhump dynamics. In this way we obtain likely masses of the components M₁=0.55±0.15M_☉ and M₂=0.047±0.013M_☉. 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.