Constructing the Secular Architecture of the Solar System

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Scientific paper

Giant planets are expected to be born on quasi-circular orbits, which are further damped by the interaction with the disc of gas from which they form and dynamical friction through planetesimal scattering, so that their eccentricities were acquired later. For a successful model that constructs the eccentricities of the planets, not only should the mean values be reproduced, but also the amplitudes of each eigenmode present in the eccentricities of the other planets.
Part I: Giant planets
To explain the secular configuration of the Jupiter-Saturn system, various scenarios were explored. Smooth migration through several mean-motion resonances between these two planets does not reproduce the current system, so that a third body is needed. Models containing just smooth migration of multiple planets also fail, and only models containing encounters between Saturn (or Jupiter) and Uranus, such as the Nice models, can reproduce the secular properties of the outer solar system. All encounters happen when PS/PJ<2.1.
Part II: Terrestrial planets
The secular motion of the terrestrial planets is complicated. Reproducing the architecture of the inner solar system in the framework of the Nice models is complicated by the secular resonance g5=g2, which occurs when PS/PJ=2.17. Since Jupiter has the current amplitude of its g5 term before this secular resonance, either Venus and Earth were eccentric in the past with a large g2 amplitude and were subsequently damped by the resonance, or Jupiter jumped over the resonance through an encounter with Uranus. Also, in the first Nice model, where Jupiter and Saturn approach the 2:1 resonance slowly, the eccentricity of Mars increases beyond 0.15 because of the resonance g5=g4. In the second Nice model, where the approach to the 2:1 resonance is fast, the effect on Mars is reduced.

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