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Paper: Conditions of Dynamical Stability for the HD160691 Planetary System
Volume: 321, Extrasolar Planets: Today and Tomorrow
Page: 349
Authors: Bois, E.; Rambaux, N.; Kiseleva-Eggleton, L.; Pilat-Lohinger, E.
Abstract: The orbits in the HD 160691 planetary system at first appeared highly unstable, but using the MEGNO and FLI techniques of global dynamics analysis in the orbital parameter space we have found a stabilizing mechanism that could be the key to its existence. In order to be dynamically stable, the HD 160691 planetary system has indeed to satisfy the following conditions: (1) a 2:1 mean motion resonance, combined with (2) an apsidal secular resonance in (3) a configuration Pc(ap) – S – Pb(ap) where the two apsidal lines are anti-aligned, and (4) specific conditions on the respective sizes of the eccentricities. High eccentricity for the outer orbit (ec > 0.52) is in particular the most probable necessary condition, while the eccentricity of the inner orbit becomes relatively unimportant when ec > 0.7.
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