Limiting the Thickness of the Solar Tachocline

Details Limiting the Thickness of the Solar Tachocline Limiting the Thickness of the Solar Tachocline

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh53c..02r&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH53C-02

Astronomy and Astrophysics

Astrophysics

[7537] Solar Physics, Astrophysics, And Astronomy / Solar And Stellar Variability, [7544] Solar Physics, Astrophysics, And Astronomy / Stellar Interiors And Dynamo Theory

Scientific paper

Axisymmetric, spherical MHD simulations coupling the convective and radiative interior of the Sun are presented. In these simulations we see the development of a tachocline and its thickness limited due to the dynamical effects of convective overshoot. These are the first simulations to self consistently couple the convective and radiative regions of the Sun and to reproduce a tachocline which is limited in vertical extent.

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