Components of the mass fluxes, Ṁ, in terms of the dependence of the anomalous resistive coefficient, α_m, for different strengths of the stellar magnetic field in the cases with fastest stellar rotation in our simulations, Ω_⋆ = 0.2Ω_br. The values of Ṁ_out and Ṁ_d are both computed at R = 12R_⋆, where the flow is most stable. The latter is computed across the disk height, and corresponds to the total mass accretion rate available for distribution in the system. The component Ṁ_SW at the same stellar rotation rate is shown together with corresponding torques in Fig. 9. Note: the y-label multiplication factor is given in the left upper corner of the panels.