Structure of magnetic fields in non-convective stars
Published in:
Monthly Notices of the Royal Astronomical Society 402,1 (2010) 345-352;
Link to original published article:
http://dx.doi.org/10.1111/j.1365-2966.2009.15876.x
Abstract
We develop a theoretical framework to construct axisymmetric magnetic equilibria in stars, consisting of both poloidal and toroidal magnetic field components. In a stationary axisymmetric configuration, the poloidal current is a function of the poloidal magnetic flux only, and thus should vanish on field lines extending outside of the star. Non-zero poloidal current (and the corresponding non-zero toroidal magnetic field) is limited to a set of toroid-shape flux surfaces fully enclosed inside the star. If we demand that there are no current sheets then on the separatrix delineating the regions of zero and finite toroidal magnetic field both the poloidal flux function (related to the toroidal component of the magnetic field) and its derivative (related to the poloidal component) should match. Thus, for a given magnetic field in the bulk of the star, the elliptical Grad-Shafranov equation that describes magnetic field structure inside the toroid is an ill-posed problem, with both Dirichlet and Newman boundary conditions and a priori unknown distribution of toroidal and poloidal electric currents. We discuss a procedure which allows to solve this ill-posed problem by adjusting the unknown current functions. We illustrate the method by constructing a number of semi-analytical equilibria connecting to outside dipole and having various poloidal current distribution on the flux surfaces closing inside the star. In particular, we find a poloidal current-carrying solution that leaves the shape of the flux function and, correspondingly, the toroidal component of the electric current, the same as in the case of no poloidal current. The equilibria discussed in this paper may have arbitrary large toroidal magnetic field, and may include a set of stable equilibria. The method developed here can also be applied to magnetic structure of differentially rotating stars, as well as to calculate velocity field in incompressible isolated fluid vortex with a swirl.
Date of this Version
2-1-2010