THREE-DIMENSIONAL MODELING OF SUPERSONIC GAS ACCRETION AND IONIZED ENVELOPE DYNAMICS IN JUPITER-LIKE PLANETS

We explore gas giant accretion in protoplanetary disks using 3D hydrodynamical simulations of a Jupiter-mass planet. Our model incorporates a non-isothermal energy equation for gas and radiation energy diffusion, enhanced by a novel radiative feedback mechanism from the planet. Key findings demonstrate supersonic gas accretion forming an ionized envelope around the planet, with its extent (0.2-0.4 of the Hill radius) influenced by radiative feedback. This ionization radius serves as a critical boundary for accretion dynamics, impacting the calculation of accretion rates and Hα emission luminosities. We show that radiative feedback significantly increases accretion rates, especially inside the ionization radius. Accretion luminosities at this radius are substantially lower than at the Hill radius, providing new perspectives for interpreting current non-detections of Hα emissions in planet formation.