The dwarf nova WX Cet: A pretender or a clone of WZ Sge?

Our CCD photometry of WX Cet on top of the large amplitude flickering characteristic to cataclysmic binaries also reveals a periodic modulation of the brightness of WX Cet with a period of 0.05827 +/- 0.00002 d. This period is derived from our data alone, but it agrees within errors with the spectroscopic orbital period (Thorstensen et al. 1996 (TPST)). During one of our observational season we observed orbital modulation of brightness of WX Cet with switching between single hump and double hump light curves. From the analysis of the spectroscopic observations of TPST we obtain likely masses of the binary components M₁ = 0.55 +/- 0.15 M_odot, M₂ = 0.047 +/- 0.013 M_odot, as well as the size of the disk and position of the hot spot.