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The population of exoplanetary systems detected by Kepler providesopportunities to refine our understanding of planet formation. Unraveling theconditions needed to produce the observed exoplanets will sallow us to makeinformed predictions as to where habitable worlds exist within the galaxy. Inthis paper, we examine using N-body simulations how the properties of planetarysystems are determined during the final stages of assembly. While accretion isa chaotic process, trends in the ensemble properties of planetary systemsprovide a memory of the initial distribution of solid mass around a star priorto accretion. We also use EPOS, the Exoplanet Population Observation Simulator,to account for detection biases and show that different accretion scenarios canbe distinguished from observations of the Kepler systems. We show that theperiod of the innermost planet, the ratio of orbital periods of adjacentplanets, and masses of the planets are determined by the total mass and radialdistribution of embryos and planetesimals at the beginning of accretion. Ingeneral, some amount of orbital damping, either via planetesimals or gas,during accretion is needed to match the whole population of exoplanets.Surprisingly, all simulated planetary systems have planets that are similar insize, showing that the "peas in a pod" pattern can be consistent with both agiant impact scenario and a planet migration scenario. The inclusion ofmaterial at distances larger than what Kepler observes has a profound impact onthe observed planetary architectures, and thus on the formation and delivery ofvolatiles to possible habitable worlds.

Earths in Other Solar Systems N-body simulations: the Role of Orbital Damping in Reproducing the Kepler Planetary Systems