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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3760
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dc.contributor.authorMarar, T. M. K-
dc.contributor.authorPadmini, V. N-
dc.contributor.authorSeetha, S-
dc.contributor.authorNarayanan Kutty, K. R-
dc.contributor.authorKasturirangan, K-
dc.contributor.authorRao, U. R-
dc.contributor.authorBhattacharyya, J. C-
dc.date.accessioned2008-09-22T11:46:08Z-
dc.date.available2008-09-22T11:46:08Z-
dc.date.issued1988-01-
dc.identifier.citationAstronomy and Astrophysics , Vol. 189, No. 1 - 2, pp. 119 - 123en
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/2248/3760-
dc.description.abstractAM CVn, an interacting binary system consisting of two helium white dwarfs, has been classified as a nova-like object. Normally it exhibits only small amplitude modulations of 0.05 mag with a 1051 s periodicity. The authors report what is believed to be for the first time, two unusually intense optical flares in AM CVn during 1985 - 87. The characteristics of the two flares in white light observed on 1985 February 24 and 1986 February 7 with Δm = 0.34 and Δm = 1.07 respectively are described. The authors estimate the maximum amount of energy released from these flares as 2.7×1036erg and suggest in the light of current models possible sites of origin of the flaring activity.en
dc.language.isoenen
dc.publisherEuropean Southern Observatoryen
dc.relation.urihttp://adsabs.harvard.edu/abs/1988A%26A...189..119Men
dc.subjectBinary starsen
dc.subjectCataclysmic variablesen
dc.subjectStellar flaresen
dc.subjectVisible spectrumen
dc.subjectWhite dwarf starsen
dc.subjectStellar modelsen
dc.subjectStellar spectrophotometryen
dc.titleFlares on AM Canum Venaticorumen
dc.typeArticleen
Appears in Collections:IIAP Publications
J.C.Bhattacharyya (1982 - 1990)

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