On the progenitor system of Nova V2491 Cygni (Research Note)

Journal article

Authors / Editors

Ribeiro, Valério

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Publication Details

Author list: Darnley MJ, Ribeiro VARM, Bode MF, Munari U

Publisher: EDP Sciences

Place: LES ULIS CEDEX A

Publication year: 2011

Journal: Astronomy & Astrophysics (0004-6361)

Journal acronym: ASTRON ASTROPHYS

Volume number: 530

Number of pages: 4

ISSN: 0004-6361

eISSN: 1432-0746

Languages: English-Great Britain (EN-GB)

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Abstract

Nova V2491 Cyg is one of just two detected pre-outburst in X-rays. The light curve of this nova exhibited a rare "re-brightening" which has been attributed by some as the system being a polar, whilst others claim that a magnetic WD is unlikely. By virtue of the nature of X-ray and spectroscopic observations the system has been proposed as a recurrent nova, however the adoption of a 0.1 day orbital period is generally seen as incompatible with such a system. In this research note we address the nature of the progenitor system and the source of the 0.1 day periodicity. Through the combination of Liverpool Telescope observations with published data and archival 2MASS data we show that V2491 Cyg, at a distance of 10.5-14 kpc, is likely to be a recurrent nova of the U Sco-class; containing a sub-giant secondary and an accretion disk, rather than accretion directly onto the poles. We show that there is little evidence, at quiescence, supporting a similar to 0.1 day periodicity, the variation seen at this stage is likely caused by flickering of a re-established accretion disk. We propose that the periodicity seen shortly after outburst is more likely related to the outburst rather than the - then obscured - binary system. Finally we address the distance to the system, and show that a significantly lower distance (similar to 2 kpc) would result in a severely under-luminous outburst, and as such favour the larger distance and the recurrent nova scenario.

Keywords

novae, cataclysmic variables, stars: individual: V2491 Cyg

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