Chemical evolution of the solar neighbourhood

dc.contributor.author	Rana, N. C
dc.date.accessioned	2007-03-21T06:33:14Z
dc.date.available	2007-03-21T06:33:14Z
dc.date.issued	1992
dc.identifier.citation	BASI, Vol. 20, pp. 21 - 40	en
dc.identifier.uri	http://hdl.handle.net/2248/1456
dc.description.abstract	The 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 -1.67	en
dc.format.extent	1647096 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	Astronomical Society of India	en
dc.subject	Chemical evolution	en
dc.title	Chemical evolution of the solar neighbourhood	en
dc.type	Article	en