Macroscopic Processes in the Solar Interior
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With the recent results of helioseismology aboard SOHO, solar models are more and more constrained (Brun, Turck-Chieze and Morel 1998 (astro-ph/9806272)). New physical processes, mainly connected to macroscopic motions, must be introduced to understand these new observations. In this poster, we present solar models including a turbulent pressure in the outer layers and mixing due to the tachocline (Spiegel and Zahn 1992). Our results lead us to conclude that: - Turbulent pressure improves the absolute value of the acoustic mode frequencies (~ 10 microHz at 4mHz), - Mixing in a tachocline thickness of 0.05 +/- 0.03 Ro (Corbard et al. 1997) looks promising.
5 pages, 7 figures To appear in SOHO6/GONG98 Proceedings "Structure and Dynamics of the Interior of the Sun and Sun-like Stars", (email: sacha.brun@cea.fr, turck@discovery.saclay.cea.fr, zahn@mokus.obspm.fr)
5 pages, 7 figures To appear in SOHO6/GONG98 Proceedings "Structure and Dynamics of the Interior of the Sun and Sun-like Stars", (email: sacha.brun@cea.fr, turck@discovery.saclay.cea.fr, zahn@mokus.obspm.fr)