Numerical simulations of magnetic relaxation in rotating stellar radiation zones

I detail the results of simulations of magnetic relaxation, as is assumed to happen in stellar radiation zones: starting from an initially stochastically organized magnetic field, this one self-organizes towards a large-scale, mainly dipolar configuration with both poloidal and toroidal components. While previous studies focused on the description of static equilibria, I include here the rotation in the numerical setup which substantially modifies the outcome of the simulations. In particular, magnetic equilibria are found, whose configuration remain stable over diffusive timescales (in general of the order of the main-sequence lifetime) rather than dynamic ones, as would be the case in presence of MHD instability. Their privileged axis are inclined with respect to the rotation axis, as observed in early-type, magnetic main sequence stars. The stationary internal flows and the dependence of the final equilibrium state on the rotation rate are described. Implications on stellar evolution are discussed. (C) 2011 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim