Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..547t&link_type=abstract
In: Proceedings of the SOHO 10/GONG 2000 Workshop: Helio- and asteroseismology at the dawn of the millennium, 2-6 October 2000,
Astronomy and Astrophysics
Astrophysics
2
Solar Models, Tachocline
Scientific paper
Solar models are presented, which include the new treatment of the diffusion-circulation coupling as discussed for halo stars by Vauclair (1999) and Théado & Vauclair (2000) and the new European Nuclear Astrophysics Compilation of REaction rates (Angulo et al. 1999). It has been known for several years (cf Richard et al. 1996) that the mixing processes below the solar convection zone must be limited to a small depth, probably due to μ-gradient effects; this is necessary to account for the constancy of the 3He/4He ratios these last 3 Gyrs, as observed from lunar rocks; it is also consistent with helioseismic results. In previous works, a critical μ-gradient was arbitrarily introduced to stop the mixing processes at a given depth. In the present models, the physics of diffusion-induced μ-gradients and their coupling with macroscopic motions is discussed and more precisely introduced.
Richard Olivier
Theado Sylvie
Vauclair Sylvie
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