Results of the 3D hydrodynamical simulation. The panels show snapshots of the density and the velocities, taken after 300 orbital periods. From left to right: perturbed gas density, radial velocity, meridional velocity, and azimuthal velocity deviations from a sub-Keplerian velocity equilibrium solution. The velocity values are in physical units, where the simulation code unit of length is re-scaled to 100 au, and the central star is a Solar-mass star. From top to bottom: r-ϕ slices of the fields at the disk midplane, r-ϕ slices of the fields at approximately three pressure scale heights (3H) above the midplane, and r-θ slices of the fields. In the left-most column plots, the circles in dashed lines indicate the location of the inner and outer buffer zones. The dotted lines in the r-ϕ slices indicate the azimuth where the r-θ slice is taken, while in the r-θ plots the dotted line indicates the location where z ~ 3H.