Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7270
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dc.contributor.authorRaj, A-
dc.contributor.authorPavana, M-
dc.contributor.authorKamath, U. S-
dc.contributor.authorAnupama, G. C-
dc.contributor.authorWalter, F. M-
dc.date.accessioned2018-04-23T04:43:09Z-
dc.date.available2018-04-23T04:43:09Z-
dc.date.issued2018-03-
dc.identifier.citationActa Astronomica, Vol. 68, No. 1, pp. 79-88en_US
dc.identifier.issn0001-5237-
dc.identifier.urihttp://hdl.handle.net/2248/7270-
dc.descriptionRestricted Accessen_US
dc.description.abstractUsing our previously reported observations, we derive some physical parameters of the moderately fast nova V2676 Oph 2012 #1. The best-fit Cloudy model of the nebular spectrum obtained on 2015 May 8 shows a hot white dwarf source with TBB≈1.0×105 K having a luminosity of 1.0×1038 erg/s. Our abundance analysis shows that the ejecta are significantly enhanced relative to solar, He/H=2.14, O/H=2.37, S/H=6.62 and Ar/H=3.25. The ejecta mass is estimated to be 1.42×10-5 M⊙. The nova showed a pronounced dust formation phase after 90 d from discovery. The J-H and H-K colors were very large as compared to other molecule- and dust-forming novae in recent years. The dust temperature and mass at two epochs have been estimated from spectral energy distribution fits to infrared photometry.en_US
dc.language.isoenen_US
dc.publisherCopernicus Foundation for Polish Astronomyen_US
dc.relation.urihttp://acta.astrouw.edu.pl/Vol68/n1/pdf/pap_68_1_4.pdf-
dc.rights© Copernicus Foundation for Polish Astronomy-
dc.subjectLine: identificationen_US
dc.subjectNovae, cataclysmic variablesen_US
dc.subjectStars: individual: V2676 Ophen_US
dc.subjectTechniques: spectroscopicen_US
dc.titleV2676 Oph: estimating physical parameters of a moderately fast novaen_US
dc.typeArticleen_US
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