Maximum radial outflow velocities (see text for details), for all cases, revealing a dependence on system parameters. The panels show variation with respect to (a) disk density, (b) stellar magnetic field energy, and (c) the strength of a vertical magnetic field (in addition to the stellar dipole field). The abscissa values in (a) and (b) are relative to the baseline case. The dotted lines are power‐law fits to the data.