The 3D Dust and Opacity Distribution of Protoplanets in Multifluid Global Simulations

Abstract The abundance and distribution of solids inside the Hill sphere are central to our understanding giant planet dichotomy. Here, we present a 3D characterization dust density, mass flux, mean opacities in envelope subthermal superthermal-mass planets. We simulate dynamics multiple species global protoplanetary disk model accounting for feedback. find that meridional flows do not effectively stir grains at scales Bondi sphere. Thus settling driven by stellar gravitational potential sets latitudinal density gradient within envelope. Not only does planet’s enhance this gradient, but also spiral wakes serve as another source asymmetry. These asymmetries substantially alter inferred Rosseland Planck opacities. In cases with moderate-to-strong settling, opacity can range from few percent more than two orders magnitude between midplane polar regions Finally, show strong introduce transition optically thick thin regimes suggest is likely occur when equilibrium scale height hundred-micron-sized particles smaller radius forming planet. This work calls into question adoption constant derived well-mixed distributions demonstrates need radiation hydrodynamics models formation account dynamics.