Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282..843m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 3, p. 843-857
Astronomy and Astrophysics
Astrophysics
18
Massive Stars, Pre-Main Sequence Stars, Stellar Convection, Stellar Evolution, Stellar Interiors, Stellar Models, Hertzsprung-Russell Diagram, Mathematical Models, Stellar Mass
Scientific paper
Two mixing schemes, overshooting and semi-convection, are studied in the framework of evolutionary models for Pop. I intermediate-mass and massive stars up to 20 solar mass. Overshooting is applied either to the core boundary, or to the boundaries of all convective zones. A generalized computation algorithm is proposed for semi-convection. The evolutionary models are computed from the quasi-hydrostatic Pre-Main-Sequence phase to the end of core helium burning. They are compared to models adopting the standard mixing scheme with no mixing beyond the Schwartzchild's limit. Overshooting, when applied to the boundaries of all convective zones, does not modify the evolutionary features of the stars. We find that semi-convection does not develop in intermediate-mass stars. In contrast, semi-convection and core overshooting completely modify the structural evolution of massive stars after central hydrogen exhaustion. The tracks followed in the H-R diagram and the times spent in different phases of evolution disfavour the models with core overshooting and favours the ones including semi-convection.
Forestini Manuel
Mowlavi Nami
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