Chemical evolution coefficients for the study of galactic evolution

Mallik, D. C. V

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dc.contributor.author	Mallik, D. C. V
dc.date.accessioned	2008-12-18T15:08:42Z
dc.date.available	2008-12-18T15:08:42Z
dc.date.issued	1981-05
dc.identifier.citation	Astrophysics and Space Science, Vol. 69, No. 1, pp. 133 - 145	en
dc.identifier.issn	0004-640X
dc.identifier.uri	http://hdl.handle.net/2248/4127
dc.description	Open Access
dc.description.abstract	A 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.iso	en	en
dc.publisher	D.Reidel Publishing Co.,	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1980Ap%26SS..69..133M	en
dc.relation.uri	http://dx.doi.org/10.1007/BF00638973	en
dc.rights	© D.Reidel Publishing Co.,
dc.subject	Chemical Evolution	en
dc.subject	Galactic Evolution	en
dc.subject	Interstellar Chemistry	en
dc.subject	Nuclear Fusion	en
dc.subject	Stellar Evolution	en
dc.subject	Stellar Mass Ejection	en
dc.subject	Abundance	en
dc.subject	Astronomical Models	en
dc.subject	Stellar Structure	en
dc.title	Chemical evolution coefficients for the study of galactic evolution	en
dc.type	Article	en