Convective overshooting in the evolution of very massive stars

Details Convective overshooting in the evolution of very massive stars Convective overshooting in the evolution of very massive stars

Aug 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...247.1063s&link_type=abstract

Astrophysical Journal, Part 1, vol. 247, Aug. 1, 1981, p. 1063-1069.

Astronomy and Astrophysics

Astrophysics

25

Convection, Mass Transfer, Stellar Evolution, Stellar Mass, Stellar Structure, Supermassive Stars, Helium, Hertzsprung-Russell Diagram, Hydrogen, Main Sequence Stars, Red Giant Stars, Stellar Envelopes, Stellar Luminosity, Stellar Models, Supergiant Stars

Scientific paper

Possible convective overshooting in stars of 30-120 solar masses are considered, including a merger between the convective core and the intermediate zone, and penetration by the outer convection zone into the hydrogen-shell region when the star is a supergiant. Convective mixing between the core and inner envelopes is found to lead to a brief renewal of hydrogen burning in the core, and a moderate widening of the main sequence bond in the H-R diagram. Deep penetration by the outer convection zone is found to force the star out of the red supergiant configuration and into a configuration near the main sequence. This would account for the apparent spread of the uppermost part of the main sequence and the concentration of luminous supergiants towards earlier spectral types. In addition, heavy mass loss need not be assumed to achieve the points of agreement, and are tentatively considered unimportant from an evolutionary point of view.

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