The turbulent diffusion phenomenon and the solar neutrino problem

Details The turbulent diffusion phenomenon and the solar neutrino problem The turbulent diffusion phenomenon and the solar neutrino problem

Sep 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980crasb.291...81s&link_type=abstract

Academie des Sciences (Paris), Comptes Rendus, Serie B - Sciences Physiques, vol. 291, no. 2, Sept. 15, 1980, p. 81-83. In Fren

Astronomy and Astrophysics

Astrophysics

3

Chemical Evolution, Solar Neutrinos, Stellar Evolution, Stellar Rotation, Turbulent Diffusion, A Stars, Abundance, Angular Momentum, Astrophysics, Chemical Composition

Scientific paper

Various indications of an astrophysical nature (distinction between Am and Ap stars, and normal A stars, lithium abundance in some giant stars, isotopic abundance ratio C-12/C-13), as well as physical phenomena (formation of limiting layers, Richardson-Townsend criterion) suggest that a weak turbulence may generate efficient processes of diffusion in rotating stars. By introducing a turbulent diffusion coefficient, a solar model is constructed which satisfies three fundamental constraints: the luminosity value at 4.6 billion years, neutrino flux, and the isotopic abundance ratio He-3/He-4 at the solar surface.

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