Volume 546, October 2012
|Number of page(s)
|Planets and planetary systems
|08 October 2012
Dissipation in planar resonant planetary systems
Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR8028, Observatoire de
77 Av. Denfert-Rochereau,
2 Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal
3 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
Accepted: 25 August 2012
Close-in planetary systems detected by the Kepler mission present an excess of period ratios that are just slightly larger than some low order resonant values. This feature occurs naturally when resonant couples undergo dissipation that damps the eccentricities. However, the resonant angles appear to librate at the end of the migration process, which is often believed to be an evidence that the systems remain in resonance. Here we provide an analytical model for the dissipation in resonant planetary systems valid for low eccentricities. We confirm that dissipation accounts for an excess of pairs that lie just aside from the nominal period ratios, as observed by the Kepler mission. In addition, by a global analysis of the phase space of the problem, we demonstrate that these final pairs are non-resonant. Indeed, the separatrices that exist in the resonant systems disappear with the dissipation, and remains only a circulation of the orbits around a single elliptical fixed point. Furthermore, the apparent libration of the resonant angles can be explained using the classical secular averaging method. We show that this artifact is only due to the severe damping of the amplitudes of the eigenmodes in the secular motion.
Key words: celestial mechanics / planets and satellites: general / planetary systems
© ESO, 2012
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