Carbon deflagrating supernovae and the chemical history of the solar neighbourhood

Details Carbon deflagrating supernovae and the chemical history of the solar neighbourhood Carbon deflagrating supernovae and the chemical history of the solar neighbourhood

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...142...13m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 142, no. 1, Jan. 1985, p. 13-20.

Astronomy and Astrophysics

Astrophysics

29

Cosmochemistry, Galactic Evolution, Stellar Evolution, Supernovae, Astronomical Models, Carbon 12, Chemical Evolution, Helium, Interstellar Matter, Iron Isotopes, Stellar Mass, Sun

Scientific paper

Yields of some heavy elements (C-12, O-16, and Fe-56) per stellar generation have been computed, by taking into account the chemical enrichment coming from carbon-deflagration in single intermediate mass stars (Type I 1/2SN) and supernova explosion in massive stars (Type II SN). It has also been assumed that the mass range of stars becoming Type I 1/2 SNe is a function of the initial stellar metal content, favoring the occurrence of these SNe in the first stellar generations. These yields, which have been found to decrease from the first stellar generations to the late ones, have been incorporated in a chemical evolution model for the solar neighborhood under different assumptions concerning the initial mass function. By means of this model, the evolution of the abundances of C-12, O-16, and Fe-56 has been followed by taking into account the delay in the chemical enrichment due to stellar lifetimes (no instantaneous recycling approximation). It has been found that iron enrichment coming from both massive and intermediate mass stars is required to explain the different evolution of iron and oxygen over the whole galactic lifetime. A functional dependence of the initial mass function on the metal content of the interstellar medium is not excluded.

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