Recurrent novae: Single degenerate progenitors of Type Ia supernovae

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