Macroscopic Processes in the Solar Interior
Abstract
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.
Cite
@article{arxiv.astro-ph/9807090,
title = {Macroscopic Processes in the Solar Interior},
author = {A. S. Brun and S. Turck-Chieze and J. P. Zahn},
journal= {arXiv preprint arXiv:astro-ph/9807090},
year = {2007}
}
Comments
5 pages, 7 figures To appear in SOHO6/GONG98 Proceedings "Structure and Dynamics of the Interior of the Sun and Sun-like Stars", (email: [email protected], [email protected], [email protected])