2001MNRAS.328..159W

The first results of a photometric survey of faint cataclysmic variables are presented. V359 Cen is an SU UMa star with a period of 112min. Even though it is observed at quiescence, the mass-transfer rate in this old nova may be sufficiently high that in such a short period system (with its implied small mass ratio) the disc may be excited into an elliptical shape with the result that the observed brightness modulation gives a superhump period rather than an orbital period. XZ Eri is an eclipsing dwarf nova with an orbital period (P_orb) of 88.1min. HY Lup has only slight variability. V351 Pup, the remnant of Nova Puppis 1991, has P_orb=2.837 h and a light curve that strongly resembles that of the magnetic Nova Cyg 1975. V630 Sgr is the first nova remnant that has both positive superhumps (P_sh=2.980 h) and eclipses (P_orb=2.831 h). The YY Tel identification is somewhat uncertain. The correct identification for CQ Vel is provided from discovery of its flickering activity. The light curve of CE-315, a recently discovered AM CVn star, shows similarities to that of GP Com, with no apparent orbital modulation.