Modeling the Rotation of the Sun: Part 1

Details Modeling the Rotation of the Sun: Part 1 Modeling the Rotation of the Sun: Part 1

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.0801a&link_type=abstract

American Astronomical Society, SPD meeting #40, #8.01; Bulletin of the American Astronomical Society, Vol. 41, p.815

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Scientific paper

The study of large-scale meridional flows is fundamental for the understanding of chemical and dynamical transport in the interior of the Sun, especially near the base of the convection zone. For instance, meridional flows originating from the convection zone and downwelling into the tachocline with significant velocities are required in theories that explain the uniform rotation of the radiative interior with the presence of a confined primordial magnetic field. Tachocline flows of a certain intensity are also necessary in some mean-field dynamo models, and are thought to contribute to the radial transport of chemical elements in the radiative zone as inferred by helioseismological observations. The question of how deeply meridional flows originating from the convection zone penetrate into the radiative zone is re-investigated by extending the simplified analytical models developed by Gilman and Miesch (2004) and Garaud & Brummell (2008). Here, we move from models considering the radiative zone only to models comprising both the radiative and the convective regions. In this first part, we present both analytical and numerical studies of the behavior of meridional flows, generated in the convection zone by a very simplified model of the convective stresses. We discuss the amplitude and depth of penetration of these flows into the radiative interior.

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