HV Virginis and WZ Sge-Type Dwarf Novae

Abstract

Abstract A dwarf nova HV Vir was observed photometrically for eight nights during an outburst in 1992 April–May. The star showed two distinct types of periodic variation: (1) 82.20-min (0.05708d) double-humped variation with decaying amplitudes during the early stage of the outburst, and (2) 83.80-min (0.05820d) superhumps in later stages. We attributed the former to “early superhumps”, which are only seen in the earliest stage of WZ Sge-type outbursts. The superhump period and evolution of the superhumps, together with general characteristics of the light curve, make HV Vir a typical WZ Sge-type dwarf nova. HV Vir also showed a large increase of the superhump period during the superoutburst. Upon recognizing the WZ Sge-type nature of an object previously considered as a nova, we present a comprehensive list of candidates for WZ Sge-type dwarf novae and related systems.