On the horseshoe drag of a low-mass planet. I - Migration in isothermal disks

TL;DR

This paper analyzes the horseshoe drag exerted on low-mass planets in isothermal disks, extending the torque estimate beyond the horseshoe region and exploring differences between globally and locally isothermal conditions.

Contribution

It introduces a formalism based on Bernoulli invariants to extend torque estimates and clarifies the effects of temperature gradients on horseshoe drag.

Findings

Horseshoe drag accounts for the entire corotation torque.

Asymmetry in the horseshoe region is caused by vortensity perturbations.

Differences in horseshoe drag between globally and locally isothermal disks are linked to vortensity flow topology.

Abstract

We investigate the unsaturated horseshoe drag exerted on a low-mass planet by an isothermal gaseous disk. In the globally isothermal case, we use a formal- ism, based on the use of a Bernoulli invariant, that takes into account pressure effects, and that extends the torque estimate to a region wider than the horse- shoe region. We find a result that is strictly identical to the standard horseshoe drag. This shows that the horseshoe drag accounts for the torque of the whole corotation region, and not only of the horseshoe region, thereby deserving to be called corotation torque. We find that evanescent waves launched downstream of the horseshoe U-turns by the perturbations of vortensity exert a feed-back on the upstream region, that render the horseshoe region asymmetric. This asymmetry scales with the vortensity gradient and with the disk's aspect ratio. It does not depend on the planetary mass, and it does not have any impact on the horseshoe drag. Since the horseshoe drag has a steep dependence on the width of the horseshoe region, we provide an adequate definition of the width that needs to be used in horseshoe drag estimates. We then consider the case of locally isothermal disks, in which the tempera- ture is constant in time but depends on the distance to the star. The horseshoe drag appears to be different from the case of a globally isothermal disk. The difference, which is due to the driving of vortensity in the vicinity of the planet, is intimately linked to the topology of the flow. We provide a descriptive inter- pretation of these effects, as well as a crude estimate of the dependency of the excess on the temperature gradient.