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Theoretical studies of massive stars. II - Evolution of a 15 solar-mass star from carbon shell burning to iron core collapseThe evolution of a Population I star of 15 solar masses is described from the carbon shell burning stage to the formation and collapse of an iron core. An unusual aspect of the evolution is that neon ignition occurs off-center and neon burning propagates inward by a series of shell flashes. The extent of the core burning is generally smaller than the Chandrasekhar mass, so that most of the nuclear energy generation occurs in shell sources. Because of degeneracy and the influence of rapid convective mixing, these shell sources are unstable and the core goes through large excursions in temperature and density. The small core also causes the shell sources to converge into a narrow mass region slightly above the Chandrasekhar mass. Thus, the final nucleosynthesis yields are generally small, with silicon being most strongly enhanced with respect to solar system abundances.
Document ID
19800050952
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Sparks, W. M.
(NASA Goddard Space Flight Center Laboratory for Astronomy and Solar Physics, Greenbelt, Md., United States)
Endal, A. S.
(Louisiana State University Baton Rouge, La., United States)
Date Acquired
August 10, 2013
Publication Date
April 1, 1980
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
80A35122
Funding Number(s)
CONTRACT_GRANT: NSF AST-78-23325
Distribution Limits
Public
Copyright
Other

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