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Over the course of last decade, the Nice model has dramatically changed ourview of the solar system's formation and early evolution. Within the context ofthis model, a transient period of planet-planet scattering is triggered bygravitational interactions between the giant planets and a massive primordialplanetesimal disk, leading to a successful reproduction of the solar system'spresent-day architecture. In typical realizations of the Nice model,self-gravity of the planetesimal disk is routinely neglected, as it poses acomputational bottleneck to the calculations. Recent analyses have shown,however, that a self-gravitating disk can exhibit behavior that is dynamicallydistinct, and this disparity may have significant implications for the solarsystem's evolutionary path. In this work, we explore this discrepancy utilizinga large suite of Nice odel simulations with and without a self-gravitatingplanetesimal disk, taking advantage of the inherently parallel nature ofgraphic processing units. Our simulations demonstrate that self-consistentmodeling of particle interactions does not lead to significantly differentfinal planetary orbits from those obtained within conventional simulations.Moreover, self-gravitating calculations show similar planetesimal evolution tonon-self-gravitating numerical experiments after dynamical instability istriggered, suggesting that the orbital clustering observed in the distantKuiper belt is unlikely to have a self-gravitational origin.

Simulations of the Solar System's Early Dynamical Evolution with a Self-Gravitating Planetesimal Disk