Theoretical studies of massive stars. II - Evolution of a 15 solar-mass star from carbon shell burning to iron core collapse

Details Theoretical studies of massive stars. II - Evolution of a 15 solar-mass star from carbon shell burning to iron core collapse Theoretical studies of massive stars. II - Evolution of a 15 solar-mass star from carbon shell burning to iron core collapse

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237..130s&link_type=abstract

Astrophysical Journal, Part 1, vol. 237, Apr. 1, 1980, p. 130-141.

Astronomy and Astrophysics

Astrophysics

15

Carbon Stars, Iron, Nuclear Reactions, Stellar Evolution, Stellar Mass, Chandrasekhar Equation, Combustion, Convective Heat Transfer, Cores, Hydrodynamics, Neon, Neutrinos, Solar System, Stellar Models, Temperature Gradients

Scientific paper

The 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.

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