  The discovery of protoplanets and circumplanetary disks provides a unique
opportunity to characterize planet formation through observations. Massive
protoplanets shape the physical and chemical structure of their host
circumstellar disk by accretion, localized emission, and disk depletion. In
this work, we study the thermal changes induced within the disk by protoplanet
accretion and synthetic predictions through hydrodynamical simulations with
post-processed radiative transfer with an emphasis on radio millimeter
emission. We explored distinct growth conditions and varied both planetary
accretion rates and the local dust-to-gas mass ratios for a protoplanet at 1200
K. The radiative transfer models show that beyond the effect of disk gaps, in
most cases, the CPD and the planet's emission locally increase the disk
temperature. Moreover, depending on the local dust-to-gas depletion and
accretion rate, the CPD presence may have detectable signatures in millimeter
emission. It also has the power to generate azimuthal asymmetries important for
continuum subtraction. Thus, if other means of detection of protoplanets are
proven, the lack of corresponding evidence at other wavelengths can set limits
on their growth timescales through a combined analysis of the local dust-to-gas
ratio and the accretion rate.
