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Recent observations of gaps and non-axisymmetric features in the dustdistributions of transition disks have been interpreted as evidence of embeddedmassive protoplanets. However, comparing the predictions of planet-diskinteraction models to the observed features has shown far from perfectagreement. This may be due to the strong approximations used for thepredictions. For example, spiral arm fitting typically uses results that arebased on low-mass planets in an isothermal gas. In this work, we describetwo-dimensional, global, hydrodynamical simulations of disks with embeddedprotoplanets, with and without the assumption of local isothermality, for arange of planet-to-star mass ratios 1-10 M_jup for a 1 M_sun star. We use thePencil Code in polar coordinates for our models. We find that the inner andouter spiral wakes of massive protoplanets (M>5 M_jup) produce significantshock heating that can trigger buoyant instabilities. These drive sustainedturbulence throughout the disk when they occur. The strength of this effectdepends strongly on the mass of the planet and the thermal relaxationtimescale; for a 10 M_jup planet embedded in a thin, purely adiabatic disk, thespirals, gaps, and vortices typically associated with planet-disk interactionsare disrupted. We find that the effect is only weakly dependent on the initialradial temperature profile. The spirals that form in disks heated by theeffects we have described may fit the spiral structures observed in transitiondisks better than the spirals predicted by linear isothermal theory.

On shocks driven by high-mass planets in radiatively inefficient disks. I. Two-dimensional global disk simulations