Variable Stars - PQ And
Type UGWZ; ZZ Ceti Click for lightcurve WZ Sagittae type subclass of UGSU dwarf novae in which the interval between super-outbursts is unusually long (>4 years) due to a very low mass-transfer rate, while normal outbursts are few or absent. They show double-waved early superhumps coincident with the orbital period (as a manifestation of the 2:1 resonance) for several days at the beginning of their outbursts (the low inclination systems may show a similar period of time without variations before the onset of ordinary superhumps). They undergo re-brightenings. Orbital periods range from 0.05 to 0.08 d. Amplitudes are larger than ~7 magnitudes. ZZ Ceti variables are non-radially pulsating white dwarfs that change their brightnesses with periods from 30 seconds to 25 minutesand amplitudes from 0.001 to 0.2 magnitudes in V. They usually show several close period values. Flares of 1 magnitude are sometimes observed; however, these may be explained by the presence of close UV Ceti companions. AAVSO Legacy Cataclysmic Variable Programme
Hills Observatory: 1 January 2013 to 26 May 2020