The Dynamical Interaction between Low-mass Planets and Dust Coagulation

TL;DR

This paper studies how low-mass planets influence dust growth and migration feedback in protoplanetary disks, revealing that planet-induced coagulation modes significantly suppress dust growth and affect migration directions under certain conditions.

Contribution

It introduces a linear analysis of coupled dust-gas dynamics showing how planetary presence alters dust coagulation and migration feedback mechanisms.

Findings

Dust growth is suppressed by planet-induced coagulation modes.

Outward migration requires a dimensionless stopping time τ ≥ 0.3.

Torque variations are caused by phase shifts in density and stopping time perturbations.

Abstract

We investigate the impact of a low-mass planet on dust coagulation, and its consequent feedback on planetary migration, using a linear analysis of the coupled dust-gas hydrodynamic equations. Dust coagulation is incorporated via a single-size approximation. In the co-orbital region of the planet, we find that the growth of dust size is significantly suppressed by planet-induced coagulation modes (CMs). This effect are less pronounced with smaller stopping times, stronger gaseous turbulence or imperfect sticking. Regarding planetary migration, we find that CMs make outward migration require $\tau \gtrsim 0.3$ ($\tau$ is dimensionless stopping time) with typical turbulent strength and dust coagulation efficiency. We demonstrate that the torque variations are reasonable and arise from phase shifts between the density and stopping time perturbations in the coagulation modes.