WZ Sge-Type Star V592 Herculis
arXiv:astro-ph/0209283 · doi:10.1093/pasj/54.6.999
Abstract
We observed the entire course of the 1998 outburst of V592 Her, which was originally reported as a nova in 1968. We have been able to construct a full light curve of the outburst, which is characterized by a rapid initial decline (0.98 mag/d), which smoothly developed into a plateau phase with a slower linear decline. We detected superhumps characteristic to SU UMa-type dwarf novae ~7 d after the optical maximum. The overall behavior of the light curve and the development of superhumps were characteristic to a WZ Sge-type dwarf nova. Combined with the past literature, we have been able to uniquely determine the superhump period to be 0.05648(2) d. From this period, together with a modern interpretation of the absolute magnitude of the outburst light curve, we conclude that the overall picture of V592 Her is not inconsistent with a lower main-sequence secondary star in contrast to a previous claim that V592 Her contains a brown dwarf.
10 pages, 7 figures, accepted for publication in Publ. Astron. Soc. Japan
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- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae
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- Variable Star Network: World Center for Transient Object Astronomy and Variable Stars
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- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. II: The Second Year (2009-2010)
- Discovery of a new dwarf nova, TSS J022216.4+412259.9: WZ Sge-type dwarf novae breaking the shortest superhump period record
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- Photometric Observations of an SU UMa-type Dwarf Nova VW Coronae Borealis during Outbursts
- A New SU UMa-Type Dwarf Nova, QW Serpentis (= TmzV46)
- Spectroscopic Observations of Twenty-one Faint Cataclysmic Variables Candidates
- 1993 Superoutburst of LL Andromedae