Stable magnetic fields in stars

Reisenegger Andreas, areisene@astro.puc.cl, Pontificia Universidad Catolica de Chile, Chile
Akgun Taner, akgun@astro.cornell.edu, Barcelona Supercomputing Center
Marchant Pablo, pimarcha@uc.cl, Pontificia Universidad Catolica de Chile
Armaza Cristobal, cyarmaza@uc.cl, Pontificia Universidad Catolica de Chile
Mastrano Alpha, alpham@unimelb.edu.au, University of Melbourne

Abstract
The magnetic field structures of neutron stars, white dwarfs, Ap, and upper-main-sequence stars are long-lived and organized on large scales. MHD simulations by Braithwaite and collaborators have shown that such configurations arise naturally from random initial conditions, and consist of linked poloidal and toroidal field components in the stellar interior. I will discuss the critical role played by the stable stratification of the stellar fluid in the stability of these structures, and generally address the conditions for this stability.