Helioseismic Tests of Solar Models

Astronomy and Astrophysics – Astrophysics

Scientific paper

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7500 Solar Physics, Astrophysics, And Astronomy, 7522 Helioseismology, 7544 Stellar Interiors And Dynamo Theory

Scientific paper

We first discuss what we could learn from an updated 1--D standard solar model including a treatment of the shear layer present at the base of the convective zone, the so called tachocline. This thin layer is related to the transition from differential rotation in the convection zone to almost uniform rotation in the radiative interior and is now clearly established by helioseismic inversions. We find that a time dependent treatment of the tachocline improves significantly the agreement between computed and observed surface chemical species, such as the 7Li as well as reduces the discrepancies between the model's internal structure and the Sun (Brun, Turck-Chièze & Zahn 1999). We then turn to 3--D spherical anelastic simulations of the solar convection performed on massively parallel computers with our ASH code. We focus our attention on the establishment of the global scale flows such as the differential rotation and the meridional circulation, by looking closely at the angular momentum transport balance and the influence of the thermal wind. By doing so, we will also make use of the accurate helioseismic data and show how the angular rotation profile in our simulations is beginning to approach the differential rotation character inferred from the observations (Brun & Toomre 2001).

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