Top panels: spatial distributions of the residual azimuthal velocity δv_ϕ = (v_ϕ − v_K)∕v_K and the ratioof radial to Keplerian velocity δv_r = v_r∕v_K in the MRI model. The data correspond to the time instance near the peak of the MRI1 burst marked in the top panel of Fig. 2 with the vertical dotted line (b). The white circles in the coordinate center represent the sink cell. The disk rotates counterclockwise. Bottom panel: corresponding azimuthally averaged radial profiles of residual velocity δv_ϕ and ratio δv_r. The red dashed line shows the ratio of radial to Keplerian velocity δu_r = u_r∕v_K for an idealized steady-state disk at the time instance immediately preceding the burst.