Snapshots of the VSI-unstable hydrodynamical simulations at the disk midplane. Shown (from top to bottom) are a simulation without an embedded planet, with an embedded Saturn-mass planet, and with a Jupiter-mass planet, and (from left to right) the gas density relative to the initial value (ρ/ρ₀), radial velocity field (v_r), meridional velocity field (v_θ), and azimuthal velocity deviations from Keplerian rotation (υ_ϕ − v_Kep). The included planets are orbiting at 100 au from the central star, marked with dotted lines in the second and third rows. The dashed lines in the first panel indicate the buffer zones applied in the hydro simulations.