Dynamical evolution of the early solar system: a history of stable and rogue planets

Explaining the current orbital structure of the planets and minor bodies in the outer solar system is an outstanding problem in planetary sciences. Based on our current understanding of planet formation within the solar system's protoplanetary disk, it is possible that multiple giant planets and many other planetary bodies formed in spatially compact configurations 4.56 Gyr ago. Motivated by previous works that favor global orbital instabilities from initial primordial systems containing five or six giant planets (the Jupiter-Saturn pair and three or four ice giants akin to Uranus/Neptune), we performed extensive N-body simulations of similar systems to better understand outer solar system formation. In particular, we investigated eight loosely stable configurations, distinct disk total masses, and the role of additional Earth-mass planets in the system. As expected, we found that several of our systems experienced orbital instabilities within ~10 Myr timescales, often resulting in the dynamical ejection of ice giants and Earth-mass planets from the solar system in similar timescales. At the end of the simulations, after 500 Myr, many resulting systems contained exactly four giant planets on stable orbits resembling the current solar system. Here, we present our preliminary results on stable and lost "rogue" planets in both non- and solar system-like final systems.