Global 3D radiation hydrodynamic simulations of proto-Jupiter’s convective envelope

The traditional core accretion model of giant planet formation, developed from 1D quasi-static models, has been challenged by the discovery of recycling flows between the planetary envelope and the disc that can slow or stall envelope accretion. We carry out 3D radiation hydrodynamic simulations with an updated opacity compilation to model the proto-Jupiter's envelope. To isolate the 3D effects of convection and recycling, we simulate both isolated spherical envelopes and envelopes embedded in discs. The envelopes are heated at given rates to achieve steady states, enabling comparisons with 1D models. We vary envelope properties to obtain both radiative and convective solutions. Using a passive scalar, we observe significant mass recycling on the orbital timescale. For a radiative envelope, recycling can only penetrate to $\sim$0.1-0.2 Hill radii, while for a convective envelope, the convective motion can ``dredge up'' the deeper part of the envelope so that the entire simulated envelope is recycled efficiently. This recycling, however, has only limited effects on the envelopes' thermal structure. The radiative envelope embedded in the disc has identical structures as the isolated envelope. The convective envelopes are also similar, following the adiabatics, except for a slightly higher density when the envelope is embedded in a disc. We introduce a modified 1D approach which can fully reproduce our 3D simulations in both the radiative and convective limits. With our updated opacity, equation of states, and 1D models, we recompute Jupiter's envelope accretion with a 10 $M_{\oplus}$ core. Consistent with prior work, the timescale to runaway accretion is shorter than the disc lifetime.