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

Published online by Cambridge University Press:  01 October 2007

Li-Yong Zhou ,
Sylvio Ferraz-Mello  and
Yi-Sui Sun
Li-Yong Zhou
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected]; [email protected]
Sylvio Ferraz-Mello
Affiliation:
Instituto de Astronômico, Geofísica, e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-900 São Paulo, Brazil email: [email protected]
Yi-Sui Sun
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China email: [email protected]; [email protected]
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Abstract

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We report in this paper the numerical simulations of the capture into the 3:1 mean-motion resonance between the planets 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 capture into resonance, the system can 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 constraints on the early dynamical evolution of orbits in the extra-solar planetary systems.

Keywords

Planetary systemscelestial mechanicsmethods: numericalmethods: analytical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 485 - 490
Copyright
Copyright © International Astronomical Union 2008

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