A test of the high-eccentricity migration scenario for close-in planets

TL;DR

This paper tests the high-eccentricity migration scenario for close-in planets by analyzing eccentricity gradients and distributions, finding evidence consistent with tidal circularization dominated by planetary dissipation and suggesting HEM relevance for Neptune-sized planets.

Contribution

The study extends previous models by constructing explicit distributions and performing backward integrations, providing new insights into the role of HEM and tidal dissipation in planet migration.

Findings

Circularization occurs outside the inner edge of the distribution.

Typical planetary tidal quality factor $Q'_{p}$ is around 10^6.

Evidence suggests HEM may influence Neptune-sized planets.

Abstract

In the high-eccentricity migration (HEM) scenario, close-in planets reach the vicinity of the central star on high-eccentricity orbits that become circularized---with a concomitant decrease in the semimajor axis---through a tidal interaction with the star. Giant planets that arrive with periastron distances that are smaller than the Roche limit $a_\mathrm{R}$ lose their gaseous envelopes, resulting in an inner edge to the surviving planets' distribution. The observational evidence for this effect, while extensive, is nonetheless somewhat ambiguous because of the effect of tidal orbital decay. Here we consider another key prediction of the HEM scenario---the existence of a spatial eccentricity gradient near the location where the circularization time becomes comparable to the planet's age for typical parameters. Previous studies already found evidence for this gradient and demonstrated that its properties are consistent with the circularization process being dominated by tidal dissipation in the planet (encapsulated by the tidal quality factor $Q^\prime_\mathrm{p}$). Our work extends these treatments by constructing explicit model distributions for comparison with the data and by carrying out backward-in-time integrations using observed system parameters. We show that circularization generally occurs outside the distribution's inner edge (which defines the boundary of the so-called sub-Jovian desert) and that typically $Q^\prime_\mathrm{p}\approx10^6$ in the circularization zone (to within a factor of 3). We also find tentative evidence for an eccentricity gradient in lower-mass planets, indicating that formation through HEM may be relevant down to Neptune scales.