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An intriguing trend among \kepler's multi-planet systems is an overabundanceof planet pairs with period ratios just wide of a mean motion resonance (MMR)and a dearth of systems just narrow of them. Traditional planet formationmodels are at odds with these observations. They are also in contrast with theperiod ratios of radial-velocity-discovered multi-planet systems which tend topile up at 2:1 MMR. We propose that gas-disk migration traps planets in a MMR.After gas dispersal, orbits of these trapped planets are altered throughinteraction with a residual planetesimal disk. We study the effects ofplanetesimal disk interactions on planet pairs trapped in 2:1 MMR using planetsof mass typical of the Kepler planet candidates (KPC) and explore large rangesfor the mass, and density profile of the planetesimal disk. We find thatplanet-planetesimal disk interactions naturally create the observed asymmetryin period-ratio distribution for large ranges of planetesimal disk and planetproperties. If the planetesimal disk mass is above a threshold of ~0.2x theplanet mass, these interactions typically disrupt MMR. Afterwards, the planetsmigrate in such a way that the final period-ratio is slightly higher than theinteger ratio corresponding to the initial MMR. Below this threshold theseinteractions typically cannot disrupt the resonance and the period ratio staysclose to the integer ratio. The threshold explains why the more massive planetpairs found by RV surveys are still in resonance. We encourage future researchto explore how significantly the associated accretion would change the planets'atmospheric and surface properties.

Planetesimal Interactions Can Explain the Mysterious Period Ratios of Small Near-Resonant Planets