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Evidence in the Solar System suggests that the giant planets underwent anepoch of radial migration that was very rapid, with an e-folding timescaleshorter than 1~Myr. It is probable that the cause of this migration was thatthe giant planets experienced an orbital instability that caused them toencounter each other, resulting in radial migration. Several works suggest thatthis dynamical instability occurred `late', long after all the planets hadformed and the solar nebula had dissipated. Assuming that the terrestrialplanets had already formed, then their orbits would have been affected by themigration of the giant planets. As a result, how did the orbits of theterrestrial planets change? And can we use this migration to obtain informationon the primordial orbits of the terrestrial planets? We directly model a largenumber of terrestrial planet systems and their response to giant planetmigration. We study the change in the Angular Momentum Deficit (AMD) of theterrstrials. We conclude that the primordial AMD should have been lower than~70\% of the current value, but higher than 10\%. We find that a scenario withfive giant planets better satisfies the orbital constraints of the terrestrialplanets. We predict that Mars was initially on an eccentric and inclined orbitwhile the orbits of Mercury, Venus and Earth were more circular and coplanar.The lower primordial dynamical excitement and the peculiar partitioning betweenplanets impose new constraints for terrestrial planet formation simulations.

Constraining the primordial orbits of the Terrestrial Planets