Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ap%26ss.143..257k&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 143, no. 2, April 1988, p. 257-268. MOESC-supported research.
Astronomy and Astrophysics
Astrophysics
4
Astronomical Models, Chemical Evolution, Cosmochemistry, Galactic Evolution, Milky Way Galaxy, Abundance, Globular Clusters, Iron, Metallicity
Scientific paper
A model of chemical evolution of the galactic halo is proposed which consists of a succession of two different evolutionary stages; each stage is characterized by a different outflow rate of gas from the star-forming region so that different metal-enrichment rates result. The low-metal stars with an Fe/H abundance ratio of less than -0.8 are formed mainly during the first 3 x 10 to the 8th yr, and most of the high-metal stars with an Fe/H abundance ratio of not less than -0.8 are formed during the succeeding 2 x 10 to the 9th yr. This model naturally explains the metallicity distribution of globular clusters in the galactic halo including both the metal-rich and the metal-poor clusters. The implications of the present model on the formation and evolution of the galactic halo are also discussed.
Kumai Yasuki
Sabano Yutaka
Tosa Makoto
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