Physics
Scientific paper
Apr 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986stin...8718486o&link_type=abstract
Unknown
Physics
A Stars, Chemical Evolution, Nuclear Fusion, Star Formation, Star Formation Rate, Stellar Mass, Supernovae, Variable Stars, Abundance, Calcium, Carbon, Magnesium, Neon, Silicon, Sulfur, Zinc
Scientific paper
The effects of a decreasing star formation rate (SFR) on the galactic abundances of elements produced in massive stars (M greater than or equal to 10 solar mass) is discussed. On the basis of a straightforward model of galactic evolution, a relation between the upper mass limit of type II supernovae (M/sub SN/) 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, are produced in solar proportions leads to a unique value of M/sub SN/ and tau. The application of this method with abundance yields from Arnett (1978) and Woosley and Weaver (1986) resuults, however, in contradicting solutions: M/sub SN/ is approximately 45 solar mass, tau = infinity, and M/sub SN/ is approximately 15 solar mass, tau = 3 x 10 to the 9th power y. Thus, in order that this approach provide an effective probe of the SFR over the history of our galaxy it is essential that converging and more accurate predictions of the consequences of stellar and supernova nucleosynthesis will be forthcoming.
Olive Keith A.
Thielemann Friederich-Karl
Truran Jame. W.
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