Diffusion near the solar core.

Details Diffusion near the solar core. Diffusion near the solar core.

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...310..982m&link_type=abstract

Astronomy and Astrophysics, v.310, p.982-991

Astronomy and Astrophysics

Astrophysics

22

Diffusion, Methods: Numerical, Sun: Oscillations

Scientific paper

Qualitative reasoning leads to the conclusion that taking into account a proper diffusion process would provide a non-standard solar model (NSSM) giving smaller neutrinos fluxes and being compatible with helioseismology data. The actual theory of the diffusion process is not approached in the present paper. It is just mentioned that a phenomenological representation of the macroscopic diffusion process by a gaussian, having its maximum D_0_ (of the order of 10^3^cm^2^/s) at a distance R_0_ (of the order of 0.2Rsun_) of the solar center and a half-width Rsunsigma (of the order of 0.04Rsun_) is acceptable. This phenomenological representation can be improved including in the complete description the microscopic diffusion coefficient. The present numerical experiment appears to show that it is, possible to decrease appreciably the difference between observational data and NSSM.

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