The Apsidal Antialignment of the HD 82943 System
arXiv:astro-ph/0301353 · doi:10.1023/A:1026193724121
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 $θ_{3}$ librates about $180^{\circ}$ in the simulations. We also use a semi-analytical model to explain the numerical results for the system under study.
8 Pages, no figures, submitted to Celestial Mechanics and Dynamical Astronomy, Proceedings of IAU 189 Colloquium(Astrophysical Tides: Effects in the Solar and Exoplanetary Systems), Sept. 2002, Nanjing, P.R. China