Improved torque formula for low and intermediate mass planetary migration

TL;DR

This paper updates the planetary migration torque formula by incorporating three-dimensional effects and dependencies on disc gradients, improving accuracy for low- and intermediate-mass planets in radiative discs.

Contribution

The authors derive a new torque formula based on 3D simulations, accounting for temperature and entropy gradients, extending validity to planets up to several tens of Earth masses.

Findings

Updated torque coefficients from 3D simulations.

Derived dependence of torque on temperature and entropy gradients.

Extended the horseshoe region width to intermediate-mass planets.

Abstract

The migration of planets on nearly circular, non-inclined orbits in protoplanetary discs is entirely described by the disc's torque. This torque is a complex function of the disc parameters, and essentially amounts to the sum of two components: the Lindblad torque and the corotation torque. Known torque formulae do not reproduce accurately the torque actually experienced in numerical simulations by low- and intermediate- mass planets in radiative discs. One of the main reasons for this inaccuracy is that these formulae have been worked out in two-dimensional analyses. Here we revisit the torque formula and update many of its dimensionless coefficients by means of tailored, three- dimensional numerical simulations. In particular, we derive the dependence of the Lindblad torque on the temperature gradient, the dependence of the corotation torque on the radial entropy gradient (and work out a suitable expression of this gradient in a three-dimensional disc). We also work out the dependence of the corotation torque on the radial temperature gradient, overlooked so far. Corotation torques are known to scale very steeply with the width of the horseshoe region. We extend the expression of this width to the domain of intermediate mass planets, so that our updated torque formula remains valid for planets up to typically several tens of Earth masses, provided these relatively massive planets do not significantly deplete their coorbital region. Our torque expression can be applied to low- and intermediate-mass planets in optically thick protoplanetary discs, as well as protomoons embedded in circumplanetary discs.