Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/20579
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dc.contributor.authorHernanz, Margarita-
dc.contributor.authorJosé, Jordi-
dc.date.accessioned2010-02-02T10:55:49Z-
dc.date.available2010-02-02T10:55:49Z-
dc.date.issued2008-10-
dc.identifier.citationNew Astronomy Reviews 52(7-10): 386-389 (2008)en_US
dc.identifier.issn1387-6473-
dc.identifier.urihttp://hdl.handle.net/10261/20579-
dc.description4 pages, 1 figure, 1 table.-- Pre-print archive.en_US
dc.description.abstractThe recurrent nova RS Oph experienced an outburst in 2006, 21 years after its previous explosion in 1985, as expected. It was observed at almost all wavelengths, and important information about its properties is still being extracted. We present theoretical models of the explosion of this fascinating object, which indicate that the mass of the accreting white dwarf should be very close to the Chandrasekhar mass, to allow for such a short recurrence period. In addition, since models suggest that this nova ejects less mass than it accretes, it is an excellent candidate for a thermonuclear supernova explosion, in about 105–107 years from now. We also analyze the emission of soft gamma-rays by RS Oph detected with the BAT instrument onboard Swift, and with the PCA onboard RXTE. We rule out that this emission has its origin in radioactive decays in the expanding nova envelope.en_US
dc.description.sponsorshipThis work has been supported by the spanish MEC and by the catalan DURSI through grants ESP2007-61593, AYA2007-66256 and 2005SGR00378, and by FEDER funds.en_US
dc.format.extent141323 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoengen_US
dc.publisherElsevieren_US
dc.rightsopenAccessen_US
dc.subjectBinariesen_US
dc.subjectCloseen_US
dc.subjectSymbioticen_US
dc.subjectNovaeen_US
dc.subjectCataclysmic variablesen_US
dc.subjectStarsen_US
dc.subjectIndividual (RS Oph)en_US
dc.subjectSupernovaeen_US
dc.subjectGeneralen_US
dc.subjectNucleosynthesisen_US
dc.subjectGamma-ray astronomyen_US
dc.titleThe recurrent nova RS Oph: A possible scenario for type Ia supernovaeen_US
dc.typeartículoen_US
dc.identifier.doi10.1016/j.newar.2008.06.017-
dc.description.peerreviewedPeer revieweden_US
dc.relation.publisherversionhttp://dx.doi.org/10.1016/j.newar.2008.06.017en_US
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
item.openairetypeartículo-
item.fulltextWith Fulltext-
item.grantfulltextopen-
item.languageiso639-1en-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.cerifentitytypePublications-
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