  Planets form in young circumstellar disks called protoplanetary disks.
However, it is still difficult to catch planet formation in-situ. Nevertheless,
from recent ALMA/SPHERE data, encouraging evidence of the direct and indirect
presence of embedded planets has been identified in disks around young stars:
co-moving point sources, gravitational perturbations, rings, cavities, and
emission dips or shadows cast on disks. The interpretation of these
observations needs a robust physical framework to deduce the complex disk
geometry. In particular, protoplanetary disk models usually assume the gas
pressure scale-height given by the ratio of the sound speed over the azimuthal
velocity $H/r = c_{s\rm }/v_{\rm k}$. By doing so, \textit{radiative} pressure
fields are often ignored, which could lead to a misinterpretation of the real
vertical structure of such disks. We follow the evolution of a gaseous disk
with an embedded Jupiter mass planet through hydrodynamical simulations,
computing the disk scale-height including radiative pressure, which was derived
from a generalization of the stellar atmosphere theory. We focus on the
vertical impact of the radiative pressure in the vicinity of circumplanetary
disks, where temperatures can reach $\gtrsim 1000$ K for an accreting planet,
and radiative forces can overcome gravitational forces from the planet. The
radiation-pressure effects create a vertical optically thick column of gas and
dust at the proto-planet location, casting a shadow in scattered light. This
mechanism could explain the peculiar illumination patterns observed in some
disks around young stars such as HD 169142 where a moving shadow has been
detected, or the extremely high aspect-ratio $H/r \sim 0.2$ observed in systems
like AB Aur and CT Cha.
