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

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.