New Insights into the Early Stage of the Galactic Chemical Evolution

Details New Insights into the Early Stage of the Galactic Chemical Evolution New Insights into the Early Stage of the Galactic Chemical Evolution

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...508l.151t&link_type=abstract

The Astrophysical Journal, Volume 508, Issue 2, pp. L151-L154.

Astronomy and Astrophysics

Astronomy

50

Galaxy: Evolution, Nuclear Reactions, Nucleosynthesis, Abundances, Galaxy: Solar Neighborhood, Stars: Abundances, Stars: Population Ii, Stars: Supernovae: General, Ism: Supernova Remnants

Scientific paper

The supernova yields of several heavy elements, including alpha-, iron-group, and r-process elements, are obtained as a function of the mass of their progenitor main-sequence stars M_ms from the abundance patterns of extremely metal-poor stars with a procedure recently proposed by Shigeyama & Tsujimoto. The ejected masses of alpha- and iron-group elements increase with M_ms, whereas more Eu is ejected from supernovae with lower M_ms. For these several heavy elements, it is shown that the average abundance ratios that are weighted by the Salpeter initial mass function coincide with the ratios observed in stars with -2<[Fe/H]<-1 within 0.1 dex. It follows that the correlations of stellar abundance ratios with the metallicity are twofold. One is the abundance ratios for [Fe/H]<-2.5 imprinted by the nucleosynthesis in individual supernovae on a timescale of ~10^7 yr, and the other, for [Fe/H]>-2, results from the mixing of the products from a whole site of the nucleosynthesis, taking place on a timescale longer than 10^9 yr.

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