Early dynamical instabilities in the giant planet systems

摘要: The observed wide eccentricity distribution of extrasolar giant planets is thought to be the result dynamical instabilities and gravitational scattering among planets. Previously, it has been assumed that orbits in planet systems become gravitationally unstable after gas nebula dispersal. It was not well understood, however, how these conditions were established first place. In this work we numerically simulate evolution three as sequentially grow Jupiter's mass, dynamically interact themselves with disk. We use hydro-dynamical code FARGO modified by implementing $N$-body integrator SyMBA. new can handle close encounters collisions between To test their stability, planetary followed SyMBA for up $10^8$ yr disk We find dynamics growing complex, because migration resonances raise orbital eccentricities, cause when still around. If occur early, removed ejections, system rearranges into a new, more stable configuration. In case, emerging from disks are expected stable, would need destabilized other means (low-mass planets, planetesimal disks, etc.). Alternatively, intrinsically upon dispersal, special timing required growth (at least some of) having near end lifetime.