Resonant structure of the outer solar system in the neighborhood of the planets

The stability of the outer solar system is studied using a new numerical me thod for detecting the chaoticity of planetary motion. We explore a large p ortion of the phase space where the outer solar system evolves and construc t dynamical maps of the regions around the Jovian planets. We show that the se regions are densely filled by two- and three-planet mean motion resonanc es that generate instabilities in planetary motion. We also show how close the actual positions of the planets are to these instabilities.