Planet-Disk Interactions and the Convective Overstability. I. Low Mass Planets

TL;DR

This study investigates how the Convective Overstability in protoplanetary disks influences the migration of low-mass planets, revealing that COS-driven vortices can significantly slow inward migration, potentially aiding planet survival.

Contribution

The paper demonstrates that COS-induced vortices in 3D hydrodynamic simulations can extend planetary migration timescales by an order of magnitude, a novel insight into planet-disk interactions.

Findings

COS creates large-scale vortices that provide positive torque kicks.

COS activity can extend migration timescales by factors of about 10.

Optically thin cooling does not produce significant torque modifications.

Abstract

Rapid inward migration driven by Type I torques threatens the survival of low-mass planets in their nascent protoplanetary disks (PPDs). Positive co-rotation torques offer a potential solution, but require viscous diffusion to remain unsaturated. However, it is unclear if (magneto)-hydrodynamic turbulence provides the necessary diffusion, and disk profiles supporting such torques are often also susceptible to the Convective Overstability (COS) for suitable gas cooling timescales. To this end, we investigate torques on low-mass planets through radially global 2D (razor-thin) and vertically unstratified 3D hydrodynamic simulations of PPDs with thermal diffusion and optically thin cooling. Our 3D models with thermal diffusion, which allows COS development, show systematically different torque behavior compared to 2D models, wherein COS is absent. In 3D, the COS saturates into large-scale, long-lived vortices that migrate radially and interact gravitationally with the embedded planet. When these vortices encounter the planet, they typically provide positive torque "kicks" counteracting inward migration, as the less-massive vortices are scattered onto horseshoe orbits by the more-massive planet. We validate our simulation methods against the theoretical framework of Paardekooper et al. (2011) and demonstrate that COS-induced torque modifications can extend migration timescales by factors of approximately 10. For plausible disk models, our results suggest that COS activity can lengthen migration timescales sufficiently to overlap with, or even exceed Super-Earth formation windows (0.1-5 Myr). In contrast, simulations with optically thin cooling do not show significant torque modifications, as COS saturates in near-axisymmetric structures without producing large-scale vortices for the disk models considered here.