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K. P. Rauch, D. P. Hamilton (U. Maryland)
We describe the initial results from a new numerical code for the integration of collisional dynamics in nearly-Keplerian systems. The program allows for a subset of the bodies to be evolved self-consistently with the remainder being treated as test particles. The algorithm is based on symplectic integration techniques and incorporates several recently explored enhancements, including potential splitting to evolve two-body close encounters and time-regularization with individual timesteps to enable flexible and efficient integration of the test particles. Amenable problems range from solar system studies to the dynamics of galactic nuclei containing massive black holes.
As a first utilization we apply the code to the problem of planet migration and resonance trapping in the early Solar System driven by the scattering and absorption of planetesimals. Both the growth of Uranus and Neptune and the orbital evolution of the four giant planets are considered, in addition to the evolution of the planetesimals themselves. We comment on the implications of the results for the initial configuration of the Oort cloud.