Migration rates of planets due to scattering of planetesimals

TL;DR

This paper models planet migration caused by scattering planetesimals, analyzing the net torque from encounters, and identifies conditions for steady, stalled, or self-regulated migration regimes.

Contribution

It provides a detailed calculation of planetesimal-driven migration, considering both close and distant encounters, and introduces conditions for different migration regimes including self-regulation.

Findings

Close and distant encounter torques have opposite signs.

Migration rate is generally lower than type-I migration due to lower solid surface density.

Self-regulated migration can occur under certain conditions.

Abstract

Planets migrate due to the recoil they experience from scattering solid (planetesimal) bodies. To first order, the torques exerted by the interior and exterior disks cancel, analogous to the cancellation of the torques from the gravitational interaction with the gas (type I migration). Assuming the dispersion-dominated regime and power-laws characterized by indices {\alpha} and {\beta} for the surface density and eccentricity profiles, we calculate the net torque on the planet. We consider both distant encounters and close (orbit-crossing) encounters. We find that the close and distant encounter torques have opposite signs with respect to their {\alpha} and {\beta} dependences; and that the torque is especially sensitive to the eccentricity gradient ({\beta}). Compared to type-I migration due to excitation of density waves, the planetesimal-driven migration rate is generally lower due to the lower surface density of solids in gas-rich disk, although this may be partially or fully offset when their eccentricity and inclination are small. Allowing for the feedback of the planet on the planetesimal disk through viscous stirring, we find that under certain conditions a self-regulated migration scenario emerges, in which the planet migrates at a steady pace that approaches the rate corresponding to the one-sided torque. If the local planetesimal disk mass to planet mass ratio is low, however, migration stalls. We quantify the boundaries separating the three migration regimes.