Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2636
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dc.contributor.authorGiridhar, S-
dc.contributor.authorKameswara Rao, N-
dc.contributor.authorLambert, D. L-
dc.date.accessioned2008-07-11T10:13:20Z-
dc.date.available2008-07-11T10:13:20Z-
dc.date.issued1994-12-
dc.identifier.citationAstrophysical Journal, Part 1, Vol. 437, No. 1, pp. 476 - 484en
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/2248/2636-
dc.description.abstractAnalysis of the RV Tauri star IW Carinae shows a photospheric composition unlike that reported previously for a few other RV Tau stars but resembling that of certain post-asymptotic giant branch stars (post-AGB) stars. IW Car is carbon-rich: several lines of C I are detected and suggest C/O greater than or = 1. The star is generally metal poor. The composition of (Fe/H) approximately -1.0, (Ca/H) approximately = -1.9 but (Zn/H) approximately 0.0 reflects that of gas of solar metallicity from which easily condensable elements have condensed into dust grains and been removed from the star's photosphere. Separation of gas and dust may have occurred in the present or recent stellar wind of IW Car. These characteristics also suggest that RV Tauri stars are post-AGB objects.en
dc.format.extent1619415 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherThe American Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/1994ApJ...437..476Gen
dc.subjectAbundanceen
dc.subjectAtomic Spectraen
dc.subjectCarbonen
dc.subjectLine Spectraen
dc.subjectStellar Compositionen
dc.subjectStellar Spectraen
dc.subjectSupergiant Starsen
dc.subjectVariable Starsen
dc.subjectAstronomical Catalogsen
dc.subjectAstronomical Spectroscopyen
dc.subjectH Alpha Lineen
dc.subjectNuclear Fusionen
dc.subjectPhotosphereen
dc.subjectVisible Spectrumen
dc.titleThe chemical composition of the RV Tauri variable IW Carinaeen
dc.typeArticleen
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