On the Stability of Additional Moons Orbiting Kepler-1625 b

TL;DR

This study uses N-body simulations to investigate the potential stability of an additional massive exomoon in the Kepler-1625 b system, considering tidal and gravitational effects, and finds stable regions for such satellites.

Contribution

It provides the first detailed dynamical analysis of the stability of a second massive exomoon in the Kepler-1625 b system using N-body simulations.

Findings

Two massive satellites can coexist around Kepler-1625 b.

Stable regions for an additional satellite are inside 25 planetary radii.

Tidal interactions and mean motion resonances contribute to satellite stability.

Abstract

Since it was proposed the exomoon candidate Kepler-1625 b-I changed the way we see satellite systems. Because of its unusual physical characteristics, many questions about the stability and origin of this candidate were raised. Currently, we have enough theoretical studies to assure that if Kepler-1625 b-I is indeed confirmed, it will be stable. The origin of this candidate was also explored. Previous works indicated that the most likely scenario is capture, even though conditions for in situ formation were also investigated. In this work, we assume that Kepler-1625 b-I is an exomoon and studied the possibility of an additional, massive exomoon being stable in the same system. To model this scenario we perform N-body simulations of a system including the planet, Kepler-1625 b-I and one extra Earth-like satellite. Based on previous results, the satellites in our system will be exposed to tidal interactions with the planet and gravitation effects due to the rotation of the planet. We found that the satellite system around Kepler-1625 b is capable of harbouring two massive satellites. The extra Earth-like satellite would be stable in different locations between the planet and Kepler-1625 b-I, with a preference for regions inside $25$ $R_p$. Our results suggest that the strong tidal interactions between the planet and the satellites is an important mechanism to assure the stability of satellites in circular orbits closer to the planet, while the 2:1 mean motion resonance between the Earth-like satellite and Kepler-1625 b-I would provide stability for satellites in wider orbits.