The 2003 Superoutburst of an SU UMa-type Dwarf Nova, GO Comae Berenices

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dc.creatorImada, Akira
dc.creatorKato, Taichi
dc.creatorUemura, Makoto
dc.creatorIshioka, Ryoko
dc.creatorKrajci, Thomas
dc.creatorSano, Yasuo
dc.creatorVanmunster, Tonny
dc.creatorStarkey, Donn R.
dc.creatorCook, Lewis M.
dc.creatorPietz, Jochen
dc.creatorNogami, Daisaku
dc.creatorYeung, Bill
dc.creatorNakajima, Kazuhiro
dc.creatorTanabe, Kenji
dc.creatorKoizumi, Mitsuo
dc.creatorTaguchi, Hiroki
dc.creatorYamada, Norimi
dc.creatorNishi, Yuichi
dc.creatorMartin, Brian
dc.creatorTorii, Ken'ichi
dc.creatorKinugasa, Kenzo
dc.creatorJones, Christopher P.
dc.date2004-12-17
dc.date.accessioned2026-07-07T02:16:20Z
dc.date.available2026-07-07T02:16:20Z
dc.descriptionWe photometrically observed the 2003 June superoutburst of GO Gom. The mean superhump period was 0.063059(13) d. The resultant data revealed that (1) the obtained light curve contained a precursor, (2) a plateau stage of the object lasted 8 days, which is remarkably shorter than that of ordinary SU UMa-type dwarf novae, and (3) the amplitude of the superoutburst was less than 5 mag, which is unpredictably small when taking into account the fact that the supercycle of GO Com is about 2800 days. In order to explain these anomalies, a mass elimination process from the accretion disk, such as evaporation, may play an important role.
dc.description11 pages, 7 figures, to appear in PASJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0412450
dc.identifierhttp://arxiv.org/abs/astro-ph/0412450
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8747
dc.subjectAstrophysics
dc.titleThe 2003 Superoutburst of an SU UMa-type Dwarf Nova, GO Comae Berenices
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