EXOA2

The orbital stability of (exo-)planetary systems is far from trivial, as chaotic diffusion can strongly affect the long-term evolution of planetary orbits. Mean‑motion and secular resonances may act as stabilizing mechanisms, constraining the range of orbital parameters compatible with current observations. A variety of additional dynamical processes further shape system architectures, including perturbations on close‑in exoplanets, resonant interactions involving giant planets, planetesimal scattering during and after formation, and episodes of planetary ejection driven by collisions or tidal disruptions.

This session aims to bring together observational, theoretical, and modeling studies that investigate the dynamical pathways of these systems, from early formation stages to mature planetary systems, and to understand how these mechanisms interplay for interpreting observed architectures and assessing the long‑term stability of both compact and widely separated planetary systems.
We welcome contributions employing numerical simulations, N-body studies, stability analyses and observational constraints.