Chemical evolution, stellar nucleosynthesis, and a variable star formation rate

Details Chemical evolution, stellar nucleosynthesis, and a variable star formation rate Chemical evolution, stellar nucleosynthesis, and a variable star formation rate

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...313..813o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 313, Feb. 15, 1987, p. 813-819.

Physics

15

Chemical Evolution, Nuclear Fusion, Star Formation, Star Formation Rate, Stellar Physics, Variable Stars, Abundance, Metallicity, Oxygen, Rates (Per Time), Supernovae

Scientific paper

The effects of a decreasing star formation rate (SFR) on the galactic abundances of elements produced in massive stars are considered. On the basis of a straightforward model of galactic evolution, relation between the upper mass limit of Type II supernovae (MSN) contributing to chemical evolution and the decline of the SFR (tau) is derived, when the oxygen abundance is determined only by massive stars. The additional requirement that all intermediate-mass elements (Ne-Ti), which are also predominantly due to nucleosynthesis in massive stars, be produced in solar proportions leads to unique values of M(SN) and tau. The application of this method with abundance yields from Arnett and from Woosley and Weaver results, however, in contradicting solutions. Thus, in order that this approach provide an effective probe of the SFR over the history of the Galaxy, it is essential that converging and more accurate predictions of the consequences of stellar and supernova nucleosynthesis will be forthcoming.

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