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Effect of planetary waves on the horseshoe region in 3D dusty gaseous disks via resonant drag instabilities

Presentation #500.04 in the session Origin of Planetary Systems (Oral Presentation)

Published onOct 23, 2023
Effect of planetary waves on the horseshoe region in 3D dusty gaseous disks via resonant drag instabilities

Resonant Drag Instabilities (RDIs) in protoplanetary disks are driven by the aerodynamic back-reaction of the dust on the gas and occur when the relative dust-gas motions resonate with a wave mode intrinsic to the gas fluid. Motivated by these findings, we study the possibility of activating the RDI in the presence of planetary waves (PWs), which can form at the edge of the horseshoe region when a low-mass planet is embedded in a gaseous disk. To this end, we conduct 3D high-resolution multifluid simulations of a dusty gaseous inviscid disk including the back-reaction of the dust on the gas. We find that, overall, the planet excites planetary waves (PWs) that propagate along the critical streamlines of the horseshoe region, while perturbing the gas vorticity. Due to resonances of the streaming motion with PWs, the RDI is triggered, and the dust density distribution develops a filamentary structure, resembling the outcome of the Streaming Instability. Our results provide the first numerical evidence of this kind of instability facilitated by the presence of an embedded planet. Remarkably, we also find that the activation of the RDI produces a widening of the horseshoe region that, depending on the mass of the planet, can result in a total positive torque exerted on the planet, leading to outward migration.

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