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Late stages of massive star evolution and nucleosynthesis [electronic resource].

Published
Upton, N.Y. : Brookhaven National Laboratory, 1986.
Oak Ridge, Tenn. : Distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy.
Physical Description
Pages: 20 : digital, PDF file
Additional Creators
Brookhaven National Laboratory and United States. Department of Energy. Office of Scientific and Technical Information
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Summary
The evolution of massive stars in the mass range of 8 to 25 M solar mass is reviewed. The effect of electron degeneracy on the gravothermal nature of stars is discussed. Depending on the stellar mass, the stars form three types of cores, namely, non-degenerate, semi-degenerate, and strongly degenerate cores. The evolution for these cases is quite distinct from each other and leads to the three different types of final fate. It is suggested that our helium star model, which is equivalent to a 25 M solar mass star, will form a relatively small mass iron core despite the faster /sup 12/C(..cap alpha..,..gamma..)/sup 16/O reaction. 50 refs., 21 figs.
Report Numbers
E 1.99:bnl-38508
E 1.99: conf-8604236-3
conf-8604236-3
bnl-38508
Subject(s)
Other Subject(s)
Note
Published through SciTech Connect.
01/01/1986.
"bnl-38508"
" conf-8604236-3"
"DE87001367"
Early universe and its evolution conference, Erice, Italy, 3 Apr 1986.
Nomoto, Ken'ichi; Hashimoto, Masa-aki.
Funding Information
AC02-76CH00016
View MARC record | catkey: 13828631