The Kepler Space Telescope and the Transiting Exoplanet Satellite Survey have discovered a wide diversity of exoplanetary system architectures. In comparison to exoplanet systems, one peculiarity in the solar system is the distinct lack of a super-Earth analog, a planet archetype prevalent in the exoplanet population. Models suggest however, that the formation of an Earth-to-Super-Earth mass planet could have readily occurred in the inner regions of the solar system (<3 AU) without the migration of the Jovian worlds. In this study, we test the consequences of such a hypothesis using a three-dimensional (3D) N-Rigid-Body integrator. Previous work employed numerical models that assumed planets and interacting bodies as point-mass particles and neglected changes in spin evolution and obliquity. These neglects of one-dimensional models may be problematic when attempting to accurately track the orbital motion of a planet. With a 3D model in which the planet is modeled as a rigid body to account for its finite size and rotation, we investigate three inner terrestrial planets over 2 Myr periods and found that an additional super-Earth sized planet between 2 and 3.5 AU would have (i) destabilized Earth’s orbit over timescales of 1 Myr, (ii) increased Mars’s obliquity by ∼55°, and (iii) perturbed the eccentricity of Venus by up to e∼0.4. Our study explores an “alternate fate” of the terrestrial planets and our results suggest that if a super-Earth had formed in the inner solar system, orbital evolution histories of many terrestrial worlds would have looked very different.
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