Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....99...97m&link_type=abstract
Astronomy and Astrophysics, vol. 99, no. 1, June 1981, p. 97-107.
Astronomy and Astrophysics
Astrophysics
114
Nuclear Fusion, Stellar Evolution, Stellar Mass Ejection, Supergiant Stars, Supernovae, Wolf-Rayet Stars, Abundance, Carbon, Heavy Elements, Helium, Hertzsprung-Russell Diagram, Mass Transfer, Oxygen, Reaction Kinetics, Red Giant Stars, Stellar Models, Stellar Structure
Scientific paper
Various aspects of the evolution of the most massive stars to red supergiants (RSG) are examined, and three cases of evolution, with initial 60 solar masses, with and without mass loss from the MS to the end of the C-burning phase, are presented as archetypal examples. Some new effects of mass loss on the internal structure, during the He- and C-burning phases, the nucleosynthesis, and the relative helium to metal Y/Z and C/O enrichments are examined. The dependence on mass loss of the lifetimes in the RSG and WR (Wolf-Rayet) stages is discussed in relation to the recent findings by Maeder et al. (1980), that the ratio NRSG/N sub WR of the numbers of these stars strongly varies with galactocentric distance and is different in the LMC and SMC. The influence of mass loss on the occurrence of supernovae by pair e(plus), e(minus) formation and the observational status of supernovae, arising from massive stars, is also analyzed. Conclusions are presented, which include the following: Red supergiants, having undergone mass loss strong enough so that their H plus C plus O cores reach some critical mass fraction (variable with initial mass), turn into WR stars during the He-burning stage.
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