Mixing versus turbulent diffusion mixing and the solar neutrino problem

Details Mixing versus turbulent diffusion mixing and the solar neutrino problem Mixing versus turbulent diffusion mixing and the solar neutrino problem

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985aipc..126...69s&link_type=abstract

IN: Solar neutrinos and neutrino astronomy; Proceedings of the Conference, Lead, SD, August 23-25, 1984 (A86-37626 17-93). New Y

Astronomy and Astrophysics

Astrophysics

4

Astrophysics, Light Elements, Solar Neutrinos, Turbulent Diffusion, Abundance, Helium Isotopes, Lithium, Stellar Composition, Turbulent Mixing

Scientific paper

A short account is given of the physical processus which can explain the presence of turbulent diffusion mixing (TDM) in the radiatively stable layers of rotating stars. The difference between full mixing and TDM is explained. In the case of the Sun, the excess of 3He carried to the center of the Sun explains the efficiency of TDM in decreasing the central temperature and thereafter the small flux of Boron neutrinos. Other consequences of TDM are described, concerning (1) the relation between the present abundance of 3He in the Galaxy and the primordial abundance (2) the abundance of lithium in main sequence stars, and (3) the possibility of using the solar seismology as a test of the effect of TDM on the μ-gradient.

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