| Issue |
EAS Publications Series
Volume 82, 2019
Astro Fluid: An International Conference in Memory of Professor Jean-Paul Zahn's Great Scientific Achievements
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|---|---|---|
| Page(s) | 365 - 371 | |
| Section | Convection and Magnetism | |
| DOI | https://doi.org/10.1051/eas/1982032 | |
| Published online | 21 June 2019 | |
A.S. Brun, S. Mathis, C. Charbonnel and B. Dubrulle (eds)
EAS Publications Series, 82 (2019) 365-371
On the stability of a general magnetic field topology in stellar radiative zones
1 Laboratoire AIM Paris-Saclay, CEA/DRF – CNRS – Université Paris Diderot, IRFU/SAp Centre de Saclay, 91191 Gif-sur-Yvette Cedex, France
2 LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
* e-mail: kyle.augustson@cea.fr
This paper provides a brief overview of the formation of stellar fossil magnetic fields and what potential instabilities may occur given certain configurations of the magnetic field. One such instability is the purely magnetic Tayler instability, which can occur for poloidal, toroidal, and mixed poloidal-toroidal axisymmetric magnetic field configurations. However, most of the magnetic field configurations observed at the surface of massive stars are non-axisymmetric. Thus, extending earlier studies in spherical geometry, we introduce a formulation for the global change in the potential energy contained in a convectively-stable region for both axisymmetric and non-axisymmetric magnetic fields.
© EAS, EDP Sciences, 2019