Hydrostatic nucleosynthesis. I. Core helium and carbon burning. II. Core neon to silicon burning and presupernova abundance yields of massive stars
The reaction network of the present examination of thermonuclear synthesis of nuclei during quasi-hydrostatic stages of the evolution of massive stars is complete up to atomic weight values of 74. The equations for temperature and density evolution are formulated in a way that renders them comparatively insensitive to specific assumptions concerning stellar convection and mixing. The first part of this work presents both the model and results of core He and C burning, for original He core masses of 1.5, 2, 4, 8, and 16 solar masses; subsequent stages, up to Si burning, are considered in a second part. The study of these later core-burning stages yields information on minimum size of reaction networks, which can be used to accurately predict the neutron excess. 94 references.
- Research Organization:
- Chicago Univ., IL; Max-Planck-Institut fuer Astrophysik, Muenich, West Germany
- OSTI ID:
- 5681628
- Journal Information:
- Astrophys. J.; (United States), Vol. 295
- Country of Publication:
- United States
- Language:
- English
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Hydrostatic nucleosynthesis. II. Core neon to silicon burning and presupernova abundance yields of massive stars
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Related Subjects
GENERAL PHYSICS
STAR EVOLUTION
NUCLEOSYNTHESIS
ABUNDANCE
CARBON
CARBON BURNING
HELIUM
MASS
NEON
OXYGEN
SILICON
ELEMENTS
FLUIDS
GASES
NONMETALS
RARE GASES
SEMIMETALS
STAR BURNING
SYNTHESIS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
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