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In radiatively inefficient, laminar protoplanetary disks, embedded planetscan excite a buoyancy response as gas gets deflected vertically near theplanet. This results in vertical oscillations that drive a vortensity growth inthe planet's corotating region, speeding up inward migration in the type-Iregime. We present a comparison between PLUTO/IDEFIX and FARGO3D using 3D,inviscid, adiabatic numerical simulations of planet-disk interaction thatfeature the buoyancy response of the disk, and show that PLUTO/IDEFIX struggleto resolve higher-order modes of the buoyancy-related oscillations, weakeningvortensity growth and the associated torque. We interpret this as a drawback oftotal-energy-conserving, finite-volume schemes. Our results indicate that avery high resolution or high-order scheme is required in shock-capturing codesin order to adequately capture this effect.

Buoyancy response of a disk to an embedded planet: a cross-code comparison at high resolution