Macroscopic Processes in the Solar Interior

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dc.creatorBrun, A. S.
dc.creatorTurck-Chieze, S.
dc.creatorZahn, J. P.
dc.date1998-07-09
dc.date.accessioned2026-07-07T02:27:22Z
dc.date.available2026-07-07T02:27:22Z
dc.descriptionWith 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.
dc.description5 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)
dc.identifierhttps://arxiv.org/abs/astro-ph/9807090
dc.identifierhttp://arxiv.org/abs/astro-ph/9807090
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/12662
dc.subjectAstrophysics
dc.titleMacroscopic Processes in the Solar Interior
dc.typetext

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