Open AccessA New SU UMa-Type Dwarf Nova, QW Serpentis (= TmzV46)
Author(s) -
Daisaku Nogami,
Makoto Uemura,
Ryoko Ishioka,
H. Iwamatsu,
Taichi Kato,
Е. П. Павленко,
A. Baklanov,
Р. Новак,
S. Kiyota,
Kenji Tanabe,
Gianluca Masi,
Lewis M. Cook,
Koichi Morikawa,
P. Schmeer
Publication year - 2004
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/56.sp1.s99
Subject(s) - physics , dwarf nova , astrophysics , luminosity , cataclysmic variable star , star (game theory) , accretion disc , astronomy , stars , white dwarf , galaxy
We report on the results of the QW Ser campaign which has been continued from2000 to 2003 by the VSNET collaboration team. Four long outbursts and manyshort ones were caught during this period. Our intensive photometricobservations revealed superhumps with a period of 0.07700(4) d during all foursuperoutbursts, proving the SU UMa nature of this star. The recurrence cyclesof the normal outbursts and the superoutbursts were measured to be $\sim$50days and 240(30) days, respectively. The change rate of the superhump periodwas -5.8x10^{-5}. The distance and the X-ray luminosity in the range of 0.5-2.4keV are estimated to be 380(60) pc and log L_x = 31.0 \pm 0.1 erg s^{-1}. Theseproperties have typical values for an SU UMa-type dwarf nova with thissuperhump period.Comment: 9 pages, 12 figures, to appear in the VSNET special issue of PAS
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