Impact of embedded circumplanetary winds on the circumstellar disk: I. Reshaping the local accretion environment

TL;DR

This study uses 3D hydrodynamic simulations to show that circumplanetary winds can significantly alter local accretion patterns and potentially limit planetary growth by redistributing material.

Contribution

It introduces a parametric wind model in simulations to analyze how circumplanetary outflows impact the circumstellar environment and planetary accretion processes.

Findings

Winds redirect accretion flows from polar to equatorial regions.

Presence of winds diminishes overall accretion rates over time.

Winds reduce the total mass available within the Hill sphere.

Abstract

The existence of winds is among the uncertainties related to the growth of giant planets. Such circumplanetary outflows have been proposed to explain kinematic and chemical structures in protoplanetary disks. We investigate the immediate impact of circumplanetary outflows on the circumstellar disk environment, the planetary vicinity, and planetary growth. We performed three-dimensional hydrodynamic simulations using \texttt{FARGO3D}, implementing a parametric wind launched from the vicinity of an embedded planet. Although the imposed configurations for the outflows do not significantly alter the global structure of the disk, they do substantially redistribute material in the vicinity of the embedded planet. In particular, the wind redirects accretion flows from polar to equatorial latitudes, resulting in variable accretion patterns over time. Although the mass accretion rate variations depend on the efficiency of the outflows, their presence diminishes the accretion rate over time and the total mass reservoir within the Hill sphere and the planet's direct vicinity, potentially slowing or limiting planetary growth.