Stellar yields as a function of initial metallicity and mass limit for black hole formation

Details Stellar yields as a function of initial metallicity and mass limit for black hole formation Stellar yields as a function of initial metallicity and mass limit for black hole formation

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...264..105m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 264, no. 1, p. 105-120.

Astronomy and Astrophysics

Astronomy

498

Black Holes (Astronomy), Metallicity, Stellar Evolution, Wolf-Rayet Stars, Galactic Evolution, H Ii Regions, Interstellar Chemistry, Stellar Mass, Stellar Mass Ejection, Stellar Models, Stellar Winds

Scientific paper

Chemical yields for studies on the chemical evolution of galaxies are derived on the basis of grids of evolutionary star models from 1 to 120 solar masses with metallicities of 0.0001 and 0.020. The wind contributions in He, C, N, O, Ne, and heavy elements are given. The total stellar yields, including the contributions from the winds, supernovae, and planetary nebulae, are also derived for helium and heavy elements. It is argued that in massive stars, at high Z, large amounts of helium and carbon are ejected into the interstellar medium before being turned into heavier elements. The nucleosynthetic production is found to depend very much on metallicity. Consideration is also given to the consequences on the yields of various values of the lowest initial mass limit MBH for black hole formation, assuming that no or little mass should be lost subsequently to the general relativistic collapse. The yields in heavy elements strongly decrease with the lowering of MBH, since then more heavy elements are swallowed up by black holes.

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