Detection of orbital and superhump periods in Nova V2574 Ophiuchi (2004)

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dc.creatorKang, Tae W.
dc.creatorRetter, Alon
dc.creatorLiu, Alex
dc.creatorRichards, Mercedes
dc.date2005-12-19
dc.date2005-12-22
dc.date.accessioned2026-07-07T11:25:07Z
dc.date.available2026-07-07T11:25:07Z
dc.descriptionWe present the results of 37 nights of CCD unfiltered photometry of nova V2574 Oph (2004) from 2004 and 2005. We find two periods of 0.14164 d (~3.40 h) and 0.14773 d (~3.55 h) in the 2005 data. The 2004 data show variability on a similar timescale, but no coherent periodicity was found. We suggest that the longer periodicity is the orbital period of the underlying binary system and that the shorter period represents a negative superhump. The 3.40 h period is about 4% shorter than the orbital period and obeys the relation between superhump period deficit and binary period. The detection of superhumps in the light curve is evidence of the presence of a precessing accretion disk in this binary system shortly after the nova outburst. From the maximum magnitude - rate of decline relation, we estimate the decay rate t_2 = 17+/-4 d and a maximum absolute visual magnitude of M_Vmax = -7.7+/-1.7 mag.
dc.description6 pages, 6 figures, 2 .sty files, AJ accepted, minor change to one of references
dc.identifierhttps://arxiv.org/abs/astro-ph/0512483
dc.identifierhttp://arxiv.org/abs/astro-ph/0512483
dc.identifierAstron.J.131:1687-1692,2006
dc.identifierdoi:10.1086/500088
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/195409
dc.subjectAstrophysics
dc.titleDetection of orbital and superhump periods in Nova V2574 Ophiuchi (2004)
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