Other
Scientific paper
Sep 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aan...357....1t&link_type=abstract
AAVSO Alert Notice 357
Other
Hs 2331+3905, Wz Sge Star, Cataclysmic Variable, Zz Cet Variable, Superhumps, Aavso International Database
Scientific paper
The WZ Sge-candidate HS 2331+3905 is currently undergoing its first observed outburst. The outburst was detected by Hiroyuki Mehara, Japan, and reported via VSNET, and confirmed by Makoto Uemura, Higashi-Hiroshima Observatory. This object went into outburst some time between JD September 3.8931 UT (a fainter-than observation at m(vis) <14.6 by Eddy Muyllaert, Oostende, Belgium) and Sep. 4.7752 UT (m(V) 14.59 by Hiroyuki Mehara, VSNET, Japan). The object has risen to the most recently reported CCD observation of m(V) 9.149 on Sep. 5.4717 UT (Martin Nicholson, Northamptonshire, UK) in approximately 24 hours. The rise of more than seven magnitudes from the quiescent level of m(V) ~ 16.4 strongly suggests that this is indeed a WZ Sge-type dwarf nova. Spectra by Boris Gaensicke reported to VSNET initially showed mixed H-Balmer emission/absorption lines, which have now transitioned to H and He pure absorption lines. HS 2331+3905 was already suspected of being a WZ Sge-class dwarf nova on the basis of its short orbital period of 81.09 minutes (0.0563 d). The white dwarf temperature is very low at T=10500 K (Araujo-Betancor et al., 2005, A&A 430, 629) and the secondary star is suspected of being a brown dwarf. These together suggest a low accretion rate, also consistent with the WZ Sge class. In addition, the white dwarf primary is known to be a pulsator of the ZZ Ceti class, making this object particularly interesting from a physical standpoint; if the outburst results in temperature or other changes in the white dwa!
rf, these may change its pulsation behavior and provide new clues for white dwarf asteroseismology. Observers are strongly encouraged to observe HS 2331+3905 intensely during this ouburst. Both visual and CCD observations are needed to follow the outburst itself. CCD time series (preferably filtered) will be needed to track the expected emergence and evolution of superhumps, and filtered CCD time series observations will be needed to measure color changes during the course of the outburst. Please submit observations to the AAVSO International Database using the name HS2331+3905.
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