Sample simulation. The solid lines mark the semimajor axis of each planet, and the shaded region goes from periastron to apastron. The three Jupiter-like planets start in near coplanar, near circular orbits. After a period of chaotic evolution but mostly stable orbits, there is a sudden instability. This leads to a period of orbit crossing and strong interactions that only ends when one of the planets is ejected from the system at t = 0.8 Myr. The remaining planets have final eccentricities of e = 0.754 (outer planet) and e = 0.938 (inner planet) at 10 Myr.