Influence of an inner disc on the orbital evolution of massive planets migrating in resonance

TL;DR

This paper investigates how an inner disc influences the orbital evolution and eccentricities of resonant giant planets, using hydrodynamic and N-body simulations, to explain observed eccentricities in exoplanetary systems.

Contribution

It demonstrates that an inner disc can provide significant eccentricity damping, helping to reproduce observed orbital parameters in resonant exoplanet systems.

Findings

Inner disc affects planetary eccentricities significantly.

Hydrodynamic simulations show inner disc's damping effect.

Reproduces orbital parameters of several resonant systems.

Abstract

The formation of resonant pairs of planets in exoplanetary systems involves planetary migration in the protoplanetary disc. After a resonant capture, the subsequent migration in this configuration leads to a large increase of planetary eccentricities if no damping mechanism is applied. This has led to the conclusion that the migration of resonant planetary systems cannot occur over large radial distances and has to be terminated sufficiently rapidly through disc dissipation. In this study, we investigate whether the presence of an inner disc might supply an eccentricity damping of the inner planet, and if this effect could explain the observed eccentricities in some systems. To investigate the influence of an inner disc, we first compute hydrodynamic simulations of giant planets orbiting with a given eccentricity around an inner gas disc, and measure the effect of the latter on the planetary orbital parameters. We then perform detailed long term calculations of the GJ 876 system. We also run N-body simulations with artificial forces on the planets mimicking the effects of the inner and outer discs. We find that the influence of the inner disc can not be neglected, and that it might be responsible for the observed eccentricities. In particular, we reproduce quite well the orbital parameters of a few systems engaged in 2:1 mean motion resonances: GJ 876, HD 73526, HD 82943 and HD 128311. Finally, we derive analytically the effect that the inner disc should have on the inner planet to reach a specific orbital configuration with a given damping effect of the outer disc on the outer planet.