Spatial distributions of the residual azimuthal velocity δv_ϕ = (v_ϕ − v_K)∕v_K (top panels) and the ratio of radial to Keplerian velocity δv_r = v_r∕v_K (bottom panels) in the clump-infall model. Left and right columns correspond to the time instances during the Clump2 and Clump3 bursts, which are marked in the right column of Fig. 7 as (b) and (d). The black contour lines outlinethe clumps, the black arrows point to the position of the clump that causes the burst, while the red arrows indicate the position of the clump that participated in the close encounter (but did not migrate to the star). The white circles in the coordinate center represent the sink cell. The disk rotates counterclockwise.