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Recent observations of the protoplanetary disk around the Herbig Be star HD100546 show two bright features in infrared (H and L' bands) at about 50 AU,with one so far unexplained. We explore the observational signatures of a highmass planet causing shock heating in order to determine if it could be thesource of the unexplained infrared feature in HD 100546. More fundamentally, weidentify and characterize planetary shocks as an extra, hitherto ignored,source of luminosity in transition disks. The RADMC-3D code is used to performdust radiative transfer calculations on the hydrodynamical disk models,including volumetric heating. A stronger shock heating rate by a factor 20would be necessary to qualitatively reproduce the morphology of the secondinfrared source. Instead, we find that the outer edge of the gap carved by theplanet heats up by about 50% relative to the initial reference temperature,which leads to an increase in the scale height. The bulge is illuminated by thecentral star, producing a lopsided feature in scattered light, as the outer gapedge shows an asymmetry in density and temperature attributable to a secondaryspiral arm launched not from the Lindblad resonances but from the 2:1resonance. We conclude that high-mass planets lead to shocks in disks that maybe directly observed, particularly at wavelengths of 10 mm or longer, but thatthey are more likely to reveal their presence in scattered light by puffing uptheir outer gap edges and exciting multiple spiral arms.

On Shocks Driven by High-mass Planets in Radiatively Inefficient Disks. III. Observational Signatures in Thermal Emission and Scattered Light