A New SU UMa-Type Dwarf Nova, QW Serpentis (= TmzV46)
arXiv:astro-ph/0310274 · doi:10.1093/pasj/56.sp1.S99
Abstract
We report on the results of the QW Ser campaign which has been continued from 2000 to 2003 by the VSNET collaboration team. Four long outbursts and many short ones were caught during this period. Our intensive photometric observations revealed superhumps with a period of 0.07700(4) d during all four superoutbursts, proving the SU UMa nature of this star. The recurrence cycles of the normal outbursts and the superoutbursts were measured to be 50 days and 240(30) days, respectively. The change rate of the superhump period was -5.8x10^{-5}. The distance and the X-ray luminosity in the range of 0.5-2.4 keV are estimated to be 380(60) pc and log L_x = 31.0 \pm 0.1 erg s^{-1}. These properties have typical values for an SU UMa-type dwarf nova with this superhump period.
9 pages, 12 figures, to appear in the VSNET special issue of PASJ
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Cited by in corpus (10)
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- Variable Star Network: World Center for Transient Object Astronomy and Variable Stars
- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. II: The Second Year (2009-2010)
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- TV Corvi Revisited: Precursor and Superhump Period Derivative Linked to the Disk Instability Model
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- Characterizing Some Gaia Alerts with LAMOST and SDSS