Main-sequence systems: orbital stability around single star hosts

TL;DR

This paper reviews methods for assessing the orbital stability of planets around single stars, highlighting advances in simulations, analytical, and machine learning approaches for understanding planetary system dynamics.

Contribution

It provides a comprehensive overview of stability studies specifically for planets orbiting single stars, including recent methodological developments.

Findings

Machine learning enhances stability predictions.

Analytical and numerical methods complement each other.

Stability insights inform planetary formation and habitability.

Abstract

Stability is one of the most fundamental aspects regarding planetary systems. It plays an important role in our understanding on the formation channel of the planetary systems, as well as their habitability. Many approaches have been adopted to determine the stability of these systems, including brute-force N-body simulations, semi-analytical calculations, and more recently machine learning methods. This allows significant advances in our understanding of planetary system dynamics, as well as providing tools to constrain unknown parameters of exoplanetary systems (assuming these systems are stable). In the following, we focus on planets around single star hosts, and we provide an overview of the studies of planetary system stability for compact multi-planet systems and hierarchical multi-planet systems.