Magnetic confinement of the solar tachocline: influence of turbulent convective motions

Details Magnetic confinement of the solar tachocline: influence of turbulent convective motions Magnetic confinement of the solar tachocline: influence of turbulent convective motions

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..271..399s&link_type=abstract

Astrophysical Dynamics: From Stars to Galaxies, Proceedings of the International Astronomical Union, IAU Symposium, Volume 271,

Astronomy and Astrophysics

Astrophysics

Sun: Magnetic Fields - Stars: Evolution - Stars : Rotation

Scientific paper

We present the results of 3D simulations, performed with the ASH code, of the nonlinear, magnetic coupling between the convective and radiative zones in the Sun, through the tachocline. Contrary to the predictions of Gough & McIntyre (1998), a fossil magnetic field, deeply buried initially in the solar interior, will penetrate into the convection zone. According to Ferraro's law of iso-rotation, the differential rotation of the convective zone will thus expand into the radiation zone, along the field lines of the poloidal field.

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