Global 3D radiation-hydrodynamic simulations of gas accretion: The opacity dependent growth of Saturn-mass planets

TL;DR

This study uses advanced 3D radiative hydrodynamics simulations to analyze how various parameters influence gas accretion rates onto Saturn-mass planets, providing insights into planet formation processes.

Contribution

It introduces a comprehensive 3D simulation framework that self-consistently models gas accretion without simplifying assumptions like mass sinks, highlighting the importance of resolution and physical parameters.

Findings

Gas accretion rates are consistent with previous studies.

Resolution of at least 10 grid cells for smoothing length is necessary.

Accretion rates align with late-stage runaway accretion expectations.

Abstract

The full spatial structure and temporal evolution of the accretion flow into the envelopes of growing gas giants in their nascent discs is only accessible in simulations. Such simulations are constrained in their approach of computing the formation of gas giants by dimensionality, resolution, consideration of self-gravity, energy treatment and the adopted opacity law. Our study explores how a number of these parameters affect that measured accretion rate of a Saturn-mass planet. We present a global 3D radiative hydrodynamics framework using the FARGOCA-code. The planet is represented by a gravitational potential with a smoothing length at the location of the planet. No mass or energy sink is used, instead luminosity and gas accretion rates are self-consistently computed. We find that the gravitational smoothing length must be resolved by at least 10 grid cells to obtain converged measurements of the gas accretion rates. Secondly, we find gas accretion rates into planetary envelopes compatible with previous studies, and continue to explain those via the structure of our planetary envelopes and their luminosities. Our measured gas accretion rates are formally in the stage of Kelvin-Helmholtz contraction due to the modest entropy loss that can be obtained over the simulation time-scale, but our accretion rates are compatible with those expected during late run-away accretion. Our detailed simulations of the gas flow into the envelope of a Saturn-mass planet provides a framework for understanding the general problem of gas accretion during planet formation and highlights circulation features that develop inside the planetary envelopes. Those circulation features feedback into the envelope energetics and can have further implications for transporting dust into the inner regions of the envelope.