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 ${\theta }_3$ 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

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• Resonances of low orders in the planetary system of HD37124
• Possible solution to the riddle of HD 82943 multiplanet system: the three-planet resonance 1:2:5?
• Dynamics of planets in retrograde mean motion resonance
• A Hybrid Mechanism Forming a 2:1 Librating-Circulating Resonant Configuration in the Planetary System
• Are retrograde resonances possible in multi-planet systems?
• Planetary Migration and Eccentricity and Inclination Resonances in Extrasolar Planetary Systems
• Conditions of Dynamical Stability for the HD 160691 Planetary System
• Orbital solutions to the HD160691 (mu Arae) Doppler signal
• Retrograde resonances in compact multi-planetary systems: a feasible stabilizing mechanism