2003/01/31 by Jianghui Ji, Ji Jianghui, Hiroshi Kinoshita +7 · 1 citation
Physics and Astronomy · #Apsidal precession #Astro and Planetary Science #Astrophysics #Astrophysics and Star Formation Studies #Celestial mechanics #Classical mechanics #Mean motion #Mechanism (biology) #Motion (physics) #Physics #Planet #Planetary system #Quantum mechanics #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1023/a:1026193724121
published as Celest.Mech.Dyn.Astron.87:113-120,2003 · 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
arxiv created 2003/02/27 · openalex publication_date 2003/09/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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.