Nucleosynthetic yields and the history of the stellar birthrate

Details Nucleosynthetic yields and the history of the stellar birthrate Nucleosynthetic yields and the history of the stellar birthrate

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....82..152w&link_type=abstract

Astronomy and Astrophysics, vol. 82, no. 1-2, Feb. 1980, p. 152-156.

Astronomy and Astrophysics

Astrophysics

13

Nuclear Fusion, O Stars, Stellar Evolution, Stellar Structure, Supernovae, Abundance, Iron, Main Sequence Stars, Milky Way Galaxy, Stellar Mass

Scientific paper

The rate of production of metals is recomputed using the constant mass stellar models of Arnett (1978) and the stellar birthrate of Miller and Scalo (1979), which has a higher birthrate for massive stars. Massive stars produce an appropriate amount of metals if the stars lose negligible mass and if the birthrate is constant. With constant mass evolution and a higher past birthrate, metals would be over-produced. Chiosi (1979) has shown that mass loss decreases the yield of massive stars. In this case massive stars can account for the observed metal abundances only if the birthrate were significantly higher in the past in contradiction to independent evidence that it is nearly constant. If massive stars do not contribute significantly to metal production, stars in the mass range of about 5-15 solar masses which produce most of the observed supernova, could account for the bulk of the heavy elements by ejecting an average of about 1.6 solar mass in metals per event. With a constant birthrate, many supernova could be of the carbon-detonation type without producing too much iron.

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