Princeton University Extrasolar Planet Discussion Group

During the early stages of giant planet formation, the proto-planet continuously exchanges mass and angular momentum with the protoplanetary disks. This exchange process is believed to happen through an extended gaseous envelope that connects the solid core with the outer regions of the planet's Hill sphere. In this talk, I will present 3D multi-fluid radiation hydrodynamics simulations of a planet embedded in a disk and characterize two different types of envelopes. I will focus on realistic cooling calculations with opacity based on self-consistent dust dynamics. In particular, I will showcase the regimes where the multifluid simulations reveal an opacity that deviates from spherical symmetry. This anisotropic opacity has important implications for the formation and contraction of the planet’s atmosphere. Finally, I will discuss my simulations in the context of protoplanetary disk observations and the detection of protoplanets.