The metallicity distribution of stars in the Galactic bulge and disc

Details The metallicity distribution of stars in the Galactic bulge and disc The metallicity distribution of stars in the Galactic bulge and disc

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.156...47k&link_type=abstract

(Instituto de Astrofisica de Canarias and Comision Interministerial de Ciencia y Tecnologia, Summer School on Evolutionary Pheno

Astronomy and Astrophysics

Astrophysics

2

Galactic Bulge, Giant Stars, K Stars, Metallicity, Chemical Evolution, Galactic Evolution, Stellar Composition

Scientific paper

The chemical evolution of the three-component system of halo-bulge-disc is calculated. If the bulge accretes primordial halo matter quickly and forms stars rapidly before the gas is ejected by a galactic wind after 10 to the 9th yr, the metallicity distribution of the bulge K-giants (Rich, 1988) is reproduced. The metal-enriched matter in a wind from the bulge is mixed with the halo gas which is accreted into the disc. The metallicity distribution of the G-dwarfs and Twarog's (1980) age-metallicity relation in the solar neighborhood can be well reproduced by assuming reasonable bulge-to-disc mass ratio.

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