FOM-Institute for Plasma-Physics Rijnhuizen, The Netherlands
submitted to the Astrophysical Journal
Axisymmetric stellar wind solutions are presented, obtained by numerically solving the ideal magnetohydrodynamic (MHD) equations. Stationary solutions are critically analysed using the knowledge of the flux functions. These flux functions enter in the general variational principle governing all axisymmetric stationary ideal MHD equilibria.
The magnetized wind solutions for (differentially) rotating stars contain both a `wind' and a `dead' zone. We illustrate the influence of the magnetic field topology on the wind acceleration pattern, by varying the coronal field strength and the extent of the dead zone. This is evident from the resulting variations in the location and appearance of the critical curves where the wind speed equals the slow, Alfvén, and fast speed. Larger dead zones cause effective, fairly isotropic acceleration to super-Alfvénic velocities as the polar, open field lines are forced to fan out rapidly with radial distance. A higher field strength moves the Alfvén transition outwards. In the ecliptic, the wind outflow is clearly modulated by the extent of the dead zone.
The combined effect of a fast stellar rotation and an equatorial `dead' zone in a bipolar field configuration can lead to efficient thermo-centrifugal equatorial winds. Such winds show both poleward and equatorward streamline bending (collimation) due to significant toroidal field pressure at mid-latitudes. We discuss how coronal mass ejections are then simulated on top of the transonic outflows.