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Many protostellar disks show central cavities, rings, or spiral arms likelycaused by low-mass stellar or planetary companions, yet few such features areconclusively tied to bodies embedded in the disks. We note that even smallfeatures on the disk's surface cast shadows, because the starlight grazes thesurface. We therefore focus on accurately computing the disk's thickness, whichdepends on its temperature. We present models with temperatures set by thebalance between starlight heating and radiative cooling, that are also invertical hydrostatic equilibrium. The planet has 20, 100, or 1000~M$_\oplus$,ranging from barely enough to perturb the disk significantly, to clearing adeep tidal gap. The hydrostatic balance strikingly alters the model disk'sappearance. The planet-carved gap's outer wall puffs up under starlightheating, throwing a shadow across the disk beyond. The shadow appears inscattered light as a dark ring that could be mistaken for a gap opened byanother more distant planet. The surface brightness contrast between outer walland shadow for the 1000-M$_\oplus$ planet is an order of magnitude greater thana model neglecting the temperature disturbances. The shadow is so deep itlargely hides the planet-launched spiral wave's outer arm. Temperaturegradients are such that outer low-mass planets undergoing orbital migrationwill converge within the shadow. Furthermore the temperature perturbationsaffect the shape, size, and contrast of features at millimeter and centimeterwavelengths. Thus radiative heating and cooling are key to the appearance ofprotostellar disks with embedded planets.

Signatures of Young Planets in the Continuum Emission From Protostellar Disks