Figure 2

Two-component outflows observed in slowly (left) and rapidly (right) rotating magnetized stars. The background shows the poloidal matter flux ${\mathbf{F}}_m=\rho {\mathbf{v}}_p$, the arrows are the poloidal velocity vectors, and the lines are sample magnetic field lines. The labels point to the main outflow components. In the left-hand panel ${\alpha }_{\nu }=0.3$ and ${\alpha }_{\eta }=0.3$ while in the right-hand panel ${\alpha }_{\nu }=0.1={\alpha }_{\eta }$.