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
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