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Paper: Superoutburst of the fifth WZ Sge-type dwarf nova, RZ Leo
Volume: 261, The Physics of Cataclysmic Variables and Related Objects
Page: 489
Authors: Ishioka, R.; Uemura, M.; Kato, T.; The Vsnet Collaboration Team
Abstract: WZ Sge stars form an extreme sub-group of SU UMa-type dwarf novae. Only four stars, WZ Sge itself, HV Vir, AL Com, and EG Cnc are established members of the WZ Sge-type. They are distinguished from normal SU UMa stars by: a very long cycle length of outbursts (years--decades), very few or no normal outburst between superoutbursts, a very large amplitude of outbursts (6--9 mag), the existence of ``early superhumps'' during the earliest stage of superoutburst, which is a photometric variation with a period extremely close to the orbital period, and a very short orbital period (80--85 min). These peculiarities are explained in the disk instability model, if we assume the extremely low viscosity in the quiescent disk. But the problem is the origin of the unusually low viscosity. The dwarf nova RZ Leo was thought to be a candidate of WZ Sge stars based on its low frequency and the large amplitude of outbursts. The optical photometry presented here confirmed that RZ Leo is a WZ Sge-type dwarf nova.
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