Hydrostatic nucleosynthesis. I - Core helium and carbon burning.

Details Hydrostatic nucleosynthesis. I - Core helium and carbon burning. Hydrostatic nucleosynthesis. I - Core helium and carbon burning.

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...295..589a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 295, Aug. 15, 1985, p. 589-619.

Astronomy and Astrophysics

Astrophysics

85

Abundance, Nuclear Fusion, Stellar Cores, Stellar Evolution, Stellar Mass, Carbon, Helium, Neon, Oxygen, Polytropic Processes, Silicon

Scientific paper

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.

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