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Recurrent novae: Single degenerate progenitors of Type Ia supernovae

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dc.contributor.author Anupama, G. C
dc.contributor.author Pavana, M
dc.date.accessioned 2021-02-07T03:59:53Z
dc.date.available 2021-02-07T03:59:53Z
dc.date.issued 2020-12
dc.identifier.citation Journal of Astrophysics and Astronomy, Vol. 41, No. 1, 43 en_US
dc.identifier.issn 0973-7758
dc.identifier.uri http://hdl.handle.net/2248/7556
dc.description Restricted Access © Springer https://doi.org/10.1007/s12036-020-09661-8 en_US
dc.description.abstract Type Ia supernovae are the result of explosive thermonuclear burning in CO white dwarfs. The progenitors of the Ia supernovae are white dwarfs in an interacting binary system. The donor companion is either a degenerate star (white dwarf) or a non-degenerate star (e.g. red giant). Recurrent novae are interacting binaries with a massive white dwarf accreting from either a main sequence, slightly evolved, or a red giant star. The white dwarf in these systems is a massive, hot white dwarf, accreting at a high rate. Recurrent novae are thought to be the most promising single degenerate progenitors of Type Ia supernovae. Presented here are the properties of a few recurrent novae based on recent outbursts. The elemental abundances and their distribution in the ejected shell are discussed. en_US
dc.language.iso en en_US
dc.publisher Springer en_US
dc.subject Type Ia supernovae en_US
dc.subject recurrent novae en_US
dc.subject abundances en_US
dc.title Recurrent novae: Single degenerate progenitors of Type Ia supernovae en_US
dc.type Article en_US

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