Physics
Scientific paper
May 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...292..222s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 292, May 1, 1985, p. 222-227.
Physics
38
Convective Flow, Core Flow, Stellar Cores, Stellar Evolution, Stellar Physics, Vortices, Hertzsprung-Russell Diagram, Main Sequence Stars, Nuclear Fusion, Stellar Mass Ejection, Stellar Models
Scientific paper
The transition from stellar evolution models with no convective core overshooting (CCO) at all to models in which homogeneous mixing due to CCO reaches far beyond the formal convective core boundary is systematically explored. Overshooting is parameterized in terms of the ratio d/H(p), where d is the distance of convective overshoot beyond the formal convective core boundary and H(p) is the local pressure scale height. It is concluded that CCO in very massive main sequence stars produces a great expansion of the stellar envelope if d/H(p) is large but not excessively large. CCO does not entirely suppress convective instability above the overshoot zone in the envelopes of main sequence stars more massive than about 15 solar masses. A general comparison of theoretically constructed isochrones for young stars with observed main sequence turnups indicates that the observed turnups are longer, brighter, and cooler at the tip than those expected on thfe basis of standard evolutionary theory.
Chin Chao-Wen
Stothers Richard B.
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