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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4127
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dc.contributor.authorMallik, D. C. V-
dc.date.accessioned2008-12-18T15:08:42Z-
dc.date.available2008-12-18T15:08:42Z-
dc.date.issued1981-05-
dc.identifier.citationAstrophysics and Space Science, Vol. 69, No. 1, pp. 133 - 145en
dc.identifier.issn0004-640X-
dc.identifier.urihttp://hdl.handle.net/2248/4127-
dc.descriptionOpen Access-
dc.description.abstractA new evaluation of chemical evolution coefficients has been made using recent stellar evolution and nucleosynthesis data. The role of the low and intermediate mass stars in galactic nucleosynthesis has been emphasized. A significant amount of He-4, C-12 and neutron-rich species is found to be contributed by these stars. Comparison with observed abundances suggests a primary origin of N-14. The simple model of galactic evolution with the new coefficients has been used to derive the ratio of helium to heavy element enrichment in the Galaxy. The new stellar evolution data do not explain the large value of this ratio that has been determined observationally.en
dc.language.isoenen
dc.publisherD.Reidel Publishing Co.,en
dc.relation.urihttp://adsabs.harvard.edu/abs/1980Ap%26SS..69..133Men
dc.relation.urihttp://dx.doi.org/10.1007/BF00638973en
dc.rights© D.Reidel Publishing Co.,-
dc.subjectChemical Evolutionen
dc.subjectGalactic Evolutionen
dc.subjectInterstellar Chemistryen
dc.subjectNuclear Fusionen
dc.subjectStellar Evolutionen
dc.subjectStellar Mass Ejectionen
dc.subjectAbundanceen
dc.subjectAstronomical Modelsen
dc.subjectStellar Structureen
dc.titleChemical evolution coefficients for the study of galactic evolutionen
dc.typeArticleen
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