Torus mass, M_d(t), relative to the black-hole mass as a function of time. The initial rapid accretion rate results in a drop of M_d that becomes partially stabilised during the subsequent evolution. Time is given in dimensionless units of GM / c³. The orbital period is close to its Keplerian value near the inner edge, i.e. about Δt(R) ≃ 100 for the material near R = R_in. Top panel: the case of spin a = 0.1 is shown for different values of magnetisation parameters β = 3 (dashed), β = 80 (dotted), and β → ∞ (i.e. a non-magnetized case; solid line). Bottom panel: as above, but for a = 0.9.