Illustration of quasi-stationarity in our magnetic case solutions, in the same (code) units as in Fig. B.2. Shown is the mass flux in the various components of the flow through the disk at r = 15R_⋆ (solid black line), onto the stellar surface (dotted blue line), and into the magnetospheric wind (dashed green line). Vertical thin lines mark the interval in which we take the average for quasi-stationary solution.