Formation and transformation of the 3:1 mean-motion resonance in 55 Cancri System

Abstract

We report in this paper the numerical simulations of the capture into the 3:1 mean-motion resonance between the planet b and c in the 55 Cancri system. The results show that this resonance can be obtained by a differential planetary migration. The moderate initial eccentricities, relatively slower migration and suitable eccentricity damping rate increase significantly the probability of being trapped in this resonance. Otherwise, the system crosses the 3:1 commensurability avoiding resonance capture, to be eventually captured into a 2:1 resonance or some other higher-order resonances. After the resonance capture, the system could jump from one orbital configuration to another one if the migration continues, making a large region of the configuration space accessible for a resonance system. These investigations help us understand the diversity of resonance configurations and put some constrains on the early dynamical evolution of orbits in the extra-solar planetary systems.

arXiv comment6 pages with 2 figures. Submitted for publication in the proceedings of IAU Symposium No.249. A paper telling much more details than this paper is under preparing

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• On the migration of a system of protoplanets
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Cited by in corpus (4)

• The 1:1 resonance in Extrasolar Systems: Migration from planetary to satellite orbits
• On the dynamics of Extrasolar Planetary Systems under dissipation. Migration of planets
• Proximity of exoplanets to first-order mean-motion resonances
• On the formation of terrestrial planets between two massive planets: The case of 55 Cancri