Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3193
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dc.contributor.authorKamath, U. S-
dc.contributor.authorAnupama, G. C-
dc.contributor.authorAshok, N. M-
dc.contributor.authorChandrasekhar, T-
dc.date.accessioned2008-08-18T11:25:17Z-
dc.date.available2008-08-18T11:25:17Z-
dc.date.issued1997-12-
dc.identifier.citationAstronomical Journal, Vol. 114, No. 6, pp. 2671 - 2678en
dc.identifier.issn0004-6256-
dc.identifier.urihttp://hdl.handle.net/2248/3193-
dc.description.abstractWe present the post-maximum optical spectroscopy and infrared photometry of Nova V1425 Aquilae 1995. The data indicate that the nova belongs to the Fe ii class and that it formed an optically thin dust shell at a very early phase compared to other dust forming novae of the same class. The total dust mass is very low with a dust-to-gas ratio of ±10/Sub -3. The optical spectrum and its evolution are similar to other Fe II novae. An extinction of EB - V 0.76 is derived from the He I line ratios and a distance of 2.7 kpc is estimated from the magnitude-decay time relations.en
dc.format.extent1113157 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAmerican Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/1997AJ....114.2671Ken
dc.subjectNOVAEen
dc.titlePost-Maximum Optical and Infrared Observations of Nova V1425 Aquilae 1995en
dc.typeArticleen
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