Standard Solar models in the Light of New Helioseismic Constraints II. Mixing Below the Convective Zone

Details Standard Solar models in the Light of New Helioseismic Constraints II. Mixing Below the Convective Zone Standard Solar models in the Light of New Helioseismic Constraints II. Mixing Below the Convective Zone

1999-06-24

arxiv.org/abs/astro-ph/9906382v1

Astrophys.J.525:1032-1041,1999

Astronomy and Astrophysics

Astrophysics

15 pages, 7 figures, to be published in ApJ (used emulateapj style for latex2e). New email for A. S. Brun: sabrun@solarz.color

Scientific paper

10.1086/307932

In previous work, we have shown that recent updated standard solar models cannot reproduce the radial profile of the sound speed at the base of the convective zone (CZ) and fail to predict the Li7 depletion. In parallel, helioseismology has shown that the transition from differential rotation in the CZ to almost uniform rotation in the radiative solar interior occurs in a shallow layer called the tachocline. This layer is presumably the seat of large scale circulation and of turbulent motions. Here, we introduce a macroscopic transport term in the structure equations, which is based on a hydrodynamical description of the tachocline proposed by Spiegel and Zahn, and we calculate the mixing induced within this layer. We discuss the influence of different parameters that represent the tachocline thickness, the Brunt-Vaissala frequency at the base of the CZ, and the time dependence of this mixing process along the Sun's evolution. We show that the introduction of such a process inhibits the microscopic diffusion by about 25%. Starting from models including a pre-main sequence evolution, we obtain: a) a good agreement with the observed photospheric chemical abundance of light elements such as He3, He4, Li7 and Be9, b) a smooth composition gradient at the base of the CZ, and c) a significant improvement of the sound speed square difference between the seismic sun and the models in this transition region, when we allow the phostospheric heavy element abundance to adjust, within the observational incertitude, due to the action of this mixing process. The impact on neutrino predictions is also discussed.

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