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A solar model with turbulent diffusion mixing: surface abundances and oscillations

Published online by Cambridge University Press:  03 August 2017

Y. Lebreton ,
G. Berthomieu  and
J. Provost
Y. Lebreton
Affiliation:
Geneva Observatory, CH-1290 Sauverny
G. Berthomieu
Affiliation:
Nice Observatory and CNRS (UA128), B.P. 139, F-06003 Nice Cedex
J. Provost
Affiliation:
Nice Observatory and CNRS (UA128), B.P. 139, F-06003 Nice Cedex

Abstract

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A solar model which includes the plausible presence of a mild mixing in the solar inner radiative zone is presented. The mixing is supposed to result from the hydrodynamical instabilities which may occur in a differentially rotating medium leading then to turbulent diffusion. The model includes up-to-date input physics and takes into account the inhibition of the turbulent motions, due to molecular weight gradients (i.e. for Mr/M⊙ < 0.5). The properties of the model are compared to the standard model properties and to observational results: this turbulent diffusion mixing (TDM) improves the results on surface abundances of the light elements (7Li, 3He) and does not reduce the solar neutrino flux relative to the standard model. Moreover preliminary results show that this TDM weakly modifies the oscillation frequencies.

Type
Chapter 2: Theory of Solar Oscillations
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 95 - 98
Copyright
Copyright © Reidel 1988 

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