The Apsidal Antialignment of the HD 82943 System
Abstract
We perform numerical simulations to explore the dynamical evolution of the HD 82943 planetary system. By simulating diverse planetary configurations, we find two mechanisms of stabilizing the system: the 2:1 mean motion resonance between the two planets can act as the first mechanism for all stable orbits. The second mechanism is a dynamical antialignment of the apsidal lines of the orbiting planets, which implies that the difference of the periastron longitudes θ3 librates about 180 in the simulations. We also use a semi-analytical model to explain the numerical results for the system under study.
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