Influence of massive planet scattering on nascent terrestrial planets

In most extrasolar planetary systems, the present orbits of known giant planets admit the existence of stable terrestrial planets. Those same giant planets, however, have typically eccentric orbits that hint at violent early dynamics less benign for low mass planet formation. Under the assumption that massive planet eccentricities are the end point of gravitational scattering in multiple planet systems, we study the evolution of the building blocks of terrestrial planets during the scattering process. We find that typically, evolutionary sequences that result in a moderately eccentric giant planet orbiting at a ≃ 2.5 AU eject over 95% of the material initially present within the habitable zone. Crossing orbits largely trigger the ejection, and leave the surviving material with a wide dispersion in semi-major axis, eccentricity and inclination. Based on these results, we predict that radial velocity follow-up of terrestrial planet systems found by Kepler will find that these are anti-correlated with the presence of eccentric giant planets orbiting at a few AU. Subject headings: solar system: formation — planets and satellites: formation — planetary systems: formation — celestial mechanics