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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4491
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dc.contributor.authorAnupama, G. C-
dc.date.accessioned2009-05-26T13:46:26Z-
dc.date.available2009-05-26T13:46:26Z-
dc.date.issued2008-
dc.identifier.citationA. Evans, M. F. Bode, T. J. O'Brien, and M. J. Darnley., RS Ophiuchi (2006) and the Recurrent Nova Phenomenon ASP Conference Series, Vol. 401, proceedings of the conference held 12 - 14 June, 2007, at Keele University, Keele, United Kingdom., pp. 31 - 41en
dc.identifier.isbn978-1-58381-674-5-
dc.identifier.urihttp://hdl.handle.net/2248/4491-
dc.descriptionRestricted Access-
dc.description.abstractRecurrent novae (RNe) form a small, but heterogeneous class of cataclysmic variables that have more than one recorded outburst. There are ten known members of this class, with six short period binaries similar to classical novae, with a main sequence or a slightly evolved secondary, while the other members of this class are long period binaries consisting of red giant secondaries, similar to symbiotic systems. The white dwarfs in RNe are believed to be massive, with the mass being close to the Chandrasekhar limit in most systems. Some of these systems are thought to be potential progenitors of type Ia supernovae.en
dc.language.isoenen
dc.publisherAstronomical Society of the Pacificen
dc.relation.ispartofseriesAstronomical Society of the Pacific Conference Series; Vol. 401-
dc.relation.urihttp://aspbooks.org/custom/publications/paper/401-0031.htmlen
dc.rights© Astronomical Society of the Pacificen
dc.subjectRecurrent novae (RNe)en
dc.subjectNova Class: Objectsen
dc.titleThe recurrent nova class of objectsen
dc.typeArticleen
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