Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1456
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dc.contributor.authorRana, N. C-
dc.date.accessioned2007-03-21T06:33:14Z-
dc.date.available2007-03-21T06:33:14Z-
dc.date.issued1992-
dc.identifier.citationBASI, Vol. 20, pp. 21 - 40en
dc.identifier.urihttp://hdl.handle.net/2248/1456-
dc.description.abstractThe study presents a simple model of the chemical evolution of the solar neighborhood with reference to the evolution and frequency distribution of a particular element - iron. The history of star formation in the solar neighborhood is consistent with no variation of its rate by more than a factor of two. The calculated and observationally estimated age-metallicity relationship agree reasonably well. The initial mass function of stars in the solar neighborhood is found to follow a power law for masses greater than about 1.5 solar masses with an index of about -1.67en
dc.format.extent1647096 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.subjectChemical evolutionen
dc.titleChemical evolution of the solar neighbourhooden
dc.typeArticleen
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