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The hydrodynamic exchange of a protoplanet's envelope material with thebackground protoplanetary disk has been proposed as one mechanism to accountfor the diversity of observed planet envelopes which range in mass fractions of~1% for super-Earths to ~90% for giants. Here we present and analyze 3Dradiation-hydrodynamics models of protoplanet envelopes to understand how theexchange of mass and energy between the protoplanet and background diskinfluences the formation process. Our protoplanet envelope simulations show anexchange of material bringing the outer <0.4Rbondi envelope to steady state.This exchange provides a continuous source of energy, which acts to increasethe observed luminosity beyond that inferred from the binding energy liberatedfrom Kelvin-Helmholtz contraction alone -- a finding important for potentialprotoplanet observations. The inner <0.4Rbondi, on the other hand, appearsinsulated -- growing in accordance with 1D quasi-static theory. We incorporatethese 3D hydrodynamic effects into an extensible 1D framework with a physicallymotivated three-layer recycling parameterization. Specializing to the case ofJupiter, recycling produces minimal changes to the growth rate with the planetstill entering runaway accretion and becoming a gas giant in ~1 Myr. Even inthe inner disk (0.1 AU), our 1D models suggest that recycling is not so robustand ubiquitous as to stop all cores from becoming giants. At the same timehowever, this recycling can delay a runaway phase by an order-of-magnitudedepending on the inner disk conditions and core mass.

Growing Planet Envelopes in Spite of Recycling Flows