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

Published online by Cambridge University Press:  12 August 2011

Antoine Strugarek ,
Allan Sacha Brun  and
Jean-Paul Zahn
Antoine Strugarek
Affiliation:
Laboratoire AIM Paris-Saclay, CEA/Irfu Université Paris-Diderot CNRS/INSU, F-91191 Gif-sur-Yvette (email: [email protected])
Allan Sacha Brun
Affiliation:
Laboratoire AIM Paris-Saclay, CEA/Irfu Université Paris-Diderot CNRS/INSU, F-91191 Gif-sur-Yvette (email: [email protected])
Jean-Paul Zahn
Affiliation:
Laboratoire AIM Paris-Saclay, CEA/Irfu Université Paris-Diderot CNRS/INSU, F-91191 Gif-sur-Yvette (email: [email protected]) LUTh, Observatoire de Paris-Meudon, France
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Abstract

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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.

Keywords

Sun: magnetic fields - stars: evolution - stars : rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 399 - 400
Copyright
Copyright © International Astronomical Union 2011

References

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