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Stellar evolution at high mass with convective core overshootingThe 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.
Document ID
19850053274
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Stothers, R. B.
(NASA Goddard Inst. for Space Studies New York, NY, United States)
Chin, C.-W.
(NASA Goddard Institute for Space Studies New York, NY, United States)
Date Acquired
August 12, 2013
Publication Date
May 1, 1985
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 292
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
85A35425
Distribution Limits
Public
Copyright
Other

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