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Impact of rotation on the geometrical configurations of fossil magnetic fields

Published online by Cambridge University Press:  23 January 2015

C. Emeriau  and
S. Mathis
C. Emeriau
Affiliation:
Laboratoire AIM Paris-Saclay, CEA/DSM - CNRS - Université Paris Diderot, IRFU/SAp Centre de Saclay, F-91191 Gif-sur-Yvette Cedex, France email: constance.emeriau@cea.fr, stephane.mathis@cea.fr
S. Mathis
Affiliation:
Laboratoire AIM Paris-Saclay, CEA/DSM - CNRS - Université Paris Diderot, IRFU/SAp Centre de Saclay, F-91191 Gif-sur-Yvette Cedex, France email: constance.emeriau@cea.fr, stephane.mathis@cea.fr
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Abstract

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The MiMeS project demonstrated that a small fraction of massive stars (around 7%) presents large-scale, stable, generally dipolar magnetic fields at their surface. These fields that do not present any evident correlations with stellar mass or rotation are supposed to be fossil remnants of the initial phases of stellar evolution. They result from the relaxation to MHD equilibrium states, during the formation of stable radiation zones, of initial fields resulting from a previous convective phase. In this work, we present new theoretical results, where we generalize previous studies by taking rotation into account. The properties of relaxed fossil fields are compared to those obtained when rotation is ignored. Consequences for magnetic fields in the radiative envelope of rotating early-type stars and their stability are finally discussed.

Keywords

magnetic fieldsMHDstars: magnetic fieldsstars: rotationstars: interiors
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 373 - 374
Copyright
Copyright © International Astronomical Union 2015 

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