EDP Sciences
Free access
Volume 397, Number 3, January III 2003
Page(s) 961 - 967
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20021543

A&A 397, 961-967 (2003)
DOI: 10.1051/0004-6361:20021543

A model of the dwarf nova WX Cet

P. Rogoziecki1 and A. Schwarzenberg-Czerny2, 1

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

(Received 15 April 2002 / 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 $\epsilon$ to constrain the mass ratio q of this CB. From time resolved spectroscopy of Thorstensen et al. we determine orbital amplitude K1 and separation $2V_{\rm d}$ of the disk emission lines as well as the S-wave amplitude $A_{\rm s}$ and relative phase $\alpha$ 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 $q-\epsilon$ relation based on superhump dynamics. In this way we obtain likely masses of the components $M_1 = 0.55\pm0.15 ~M_{\odot}$ and $M_2 = 0.047\pm0.013 ~M_{\odot}$. 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

Offprint request: P. Rogoziecki, progoz@moon.astro.amu.edu.pl

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