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We carry out local three dimensional (3D) hydrodynamic simulations ofplanet-disk interaction in stratified disks with varied thermodynamicproperties. We find that whenever the Brunt-Vaisala frequency (N) in the diskis nonzero, the planet exerts a strong torque on the disk in the vicinity ofthe planet, with a reduction in the traditional "torque cutoff". In particular,this is true for adiabatic perturbations in disks with isothermal densitystructure, as should be typical for centrally irradiated protoplanetary disks.We identify this torque with buoyancy waves, which are excited (when N isnon-zero) close to the planet, within one disk scale height from its orbit.These waves give rise to density perturbations with a characteristic 3D spatialpattern which is in close agreement with the linear dispersion relation forbuoyancy waves. The torque due to these waves can amount to as much as severaltens of per cent of the total planetary torque, which is not expected based onanalytical calculations limited to axisymmetric or low-m modes. Buoyancy wavesshould be ubiquitous around planets in the inner, dense regions ofprotoplanetary disks, where they might possibly affect planet migration.

Planet-Disk interaction in 3D: the importance of buoyancy waves