On the evolution of a one-solar-mass star with a periodically mixed core

Details On the evolution of a one-solar-mass star with a periodically mixed core On the evolution of a one-solar-mass star with a periodically mixed core

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....47..137g&link_type=abstract

Astronomy and Astrophysics, vol. 47, no. 1, Feb. 1976, p. 137-141.

Astronomy and Astrophysics

Astrophysics

3

Astronomical Models, Neutrinos, Solar Corpuscular Radiation, Stellar Evolution, Stellar Mass, Stellar Structure, Cores, Mixing, Solar Flux, Structural Stability, Thermal Stability

Scientific paper

To solve the neutrino problem, Dilke and Gough (1972) have suggested that the vibrational instability of g(plus) modes of nonradial oscillation may be the cause of recurrent mixing in the sun. Supposing this to be correct, the evolution of the sun is completely different from the standard one. Unmixed solar models are stable when older than 3 billion years. It is therefore necessary to check whether in the modified evolution, instabilities still exist at the solar age. They do, provided that the mass fraction of the mixed core is large enough. However, the neutrino flux at its minimum during a thermal pulse occurring at the solar age remains too high. Constraints imposed by ice-age records are also discussed.

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