Open AccessWZ Sge-Type Star V592 Herculis
Author(s) -
Taichi Kato,
Makoto Uemura,
Katsura Matsumoto,
Timo Kinnunen,
G. J. Garradd,
Gianluca Masi,
H. Yamaoka
Publication year - 2002
Publication title -
publications of the astronomical society of japan
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.99
H-Index - 110
eISSN - 2053-051X
pISSN - 0004-6264
DOI - 10.1093/pasj/54.6.999
Subject(s) - physics , light curve , astrophysics , dwarf nova , astronomy , plateau (mathematics) , star (game theory) , cataclysmic variable star , nova (rocket) , accretion disc , white dwarf , stars , aeronautics , mathematics , mathematical analysis , engineering
We observed the entire course of the 1998 outburst of V592 Her, which wasoriginally reported as a nova in 1968. We have been able to construct a fulllight 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 slowerlinear decline. We detected superhumps characteristic to SU UMa-type dwarfnovae ~7 d after the optical maximum. The overall behavior of the light curveand the development of superhumps were characteristic to a WZ Sge-type dwarfnova. Combined with the past literature, we have been able to uniquelydetermine the superhump period to be 0.05648(2) d. From this period, togetherwith a modern interpretation of the absolute magnitude of the outburst lightcurve, we conclude that the overall picture of V592 Her is not inconsistentwith a lower main-sequence secondary star in contrast to a previous claim thatV592 Her contains a brown dwarf.Comment: 10 pages, 7 figures, accepted for publication in Publ. Astron. Soc. Japa
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