Limits on orbit crossing planetesimals in the resonant multiple planet system, KOI-730

Abstract

A fraction of multiple planet candidate systems discovered from transits by the Kepler mission contain pairs of planet candidates that are in orbital resonance or are spaced slightly too far apart to be in resonance. We focus here on the four planet system, KOI 730, that has planet periods satisfying the ratios 8:6:4:3. By numerically integrating four planets initially in this resonant configuration in proximity to an initially exterior cold planetesimal disk, we find that of the order of a Mars mass of planet-orbit-crossing planetesimals is sufficient to pull this system out of resonance. Approximately one Earth mass of planet-orbit-crossing planetesimals increases the interplanetary spacings sufficiently to resemble the multiple planet candidate Kepler systems that lie just outside of resonance. This suggests that the closely spaced multiple planet Kepler systems, host only low mass debris disks or their debris disks have been extremely stable. We find that the planetary inclinations increase as a function of the mass in planetesimals that have crossed the orbits of the planets. If systems are left at zero inclination and in resonant chains after depletion of the gas disk then we would expect a correlation between distance to resonance and mutual planetary inclinations. This may make it possible to differentiate between dynamical mechanisms that account for the fraction of multiple planet systems just outside of resonance.

7 pages, 2 figures, 2 tables

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• Tides Alone Cannot Explain Kepler Planets Close to 2:1 MMR
• The Scattered Disc of HR 8799
• The orbital architecture and debris disks of the HR 8799 planetary system
• A linear distribution of orbits in compact planetary systems?
• Two Super-Earths in the 3:2 MMR around KOI-1599
• The origin and 9:7 MMR dynamics of the Kepler-29 system
• On the migration of three planets in a protoplanetary disc and the formation of chains of mean motion resonances
• The architecture and formation of the Kepler-30 planetary system
• Effects of Planetesimal Accretion on the Thermal and Structural Evolution of Sub-Neptunes
• On the migration-induced formation of the 9:7 mean motion resonance