Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993basi...21..361b&link_type=abstract
Astronomical Society of India, Bulletin (ISSN 0304-9523), vol. 21, no. 3-4, p. 361-362
Astronomy and Astrophysics
Astronomy
Chemical Evolution, Interstellar Gas, Iron, Milky Way Galaxy, Star Formation, Stellar Evolution, Abundance, Accretion Disks, Mass Distribution, Metallicity
Scientific paper
In this thesis we have studied the evolution of gas and iron in the Galaxy. Before modeling the chemical evolution of the Galaxy, we looked into some important constraints and inputs to evolution models. We first derived the age-metallicity relation (AMR) of stars in the solar neighborhood by combining the observed history of the star formation rate of Soderblom et al. (1991) and the metallicity distribution of stars of Pagel (1989). The AMR thus derived is almost linear on a logarithmic metallicity scale after the first two Gyrs, although there is a small, almost periodic variation on this trend. We have also corrected the data of Soderblom et al. (1991) for the increase of the scale heights of stars with age to find the actual variation of the star formation rate per unit area of the disc. We find this correction makes the observed star formation history consistent with a nearly constant star formation rate (Rana & Basu 1992).
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