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