Computer Science – Numerical Analysis
Scientific paper
Mar 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....96....1s&link_type=abstract
Astronomy and Astrophysics, vol. 96, no. 1-2, Mar. 1981, p. 1-16.
Computer Science
Numerical Analysis
125
Solar Neutrinos, Stellar Evolution, Stellar Models, Turbulent Diffusion, Turbulent Mixing, Abundance, Helium Isotopes, Hydrogen, Mathematical Models, Numerical Analysis, Reynolds Number, Stellar Luminosity, Stellar Physics, Stellar Structure, Surface Properties, Transport Properties
Scientific paper
The effects of turbulent diffusion, which is due to a mild turbulence induced by instabilities in radiative stable zones, are investigated for their consequences on stellar evolution. Numerical evolutionary models for a one-solar-mass star are computed on the basis of appropriate stellar physics and a detailed treatment of the changes in the abundances of H-1, He-3, and He-4 arising from both turbulent diffusion and nuclear reactions. It is noted that the radiative and molecular viscosities are included in the transport coefficients. The main observational restraints on solar models, that is, the solar luminosity, the neutrino flux, and the surface (He-3/He-4) ratio, are examined.
Angrand F.
Glowinski Roland
Maeder Andre
Schatzman Evry
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