Jupiter and Super-Earth embedded in a gaseous disc

TL;DR

This study explores how a Jupiter and a Super-Earth interact and migrate within a gaseous protoplanetary disc, revealing conditions for resonance capture and stability through hydrodynamical simulations.

Contribution

It provides new insights into the orbital evolution and resonance capture of a Super-Earth and Jupiter in a gaseous disc using detailed 2D hydrodynamical models.

Findings

Jupiter captures Super-Earth into 3:2 or 4:3 resonances.

Resonance stability depends on initial positions and eccentricity.

Super-Earth can be scattered if initial conditions are not favorable.

Abstract

In this paper we investigate the evolution of a pair of interacting planets - a Jupiter mass planet and a Super-Earth with the 5.5 Earth masses - orbiting a Solar type star and embedded in a gaseous protoplanetary disc. We focus on the effects of type I and II orbital migrations, caused by the planet-disc interaction, leading to the Super-Earth capture in first order mean motion resonances by the Jupiter. The stability of the resulting resonant system in which the Super-Earth is on the internal orbit relatively to the Jupiter has been studied numerically by means of full 2D hydrodynamical simulations. Our main motivation is to determine the Super-Earth behaviour in the presence of the gas giant in the system. It has been found that the Jupiter captures the Super-Earth into the interior 3:2 or 4:3 mean motion resonances and the stability of such configurations depends on the initial planet positions and eccentricity evolution. If the initial separation of planet orbits is larger or close to that required for the exact resonance than the final outcome is the migration of the pair of planets with the rate similar to that of the gas giant at least for time of our simulations. Otherwise we observe a scattering of the Super-Earth from the disc. The evolution of planets immersed in the gaseous disc has been compared with their behaviour in the case of the classical three-body problem when the disc is absent.