Fig. 6

Evolution of the orbital parameters for three different fits, stable for at least 108 years. The best 2:1 MMR fit (left panels), the best stable fit from the low-eccentricity region (middle panels), and the fit with the most circular orbits (right panels). In the 2:1 MMR fit the gravitational perturbation between the planets is much larger than in the other two cases. It is easy to see that eccentricities for given epochs can be much larger than their values at the initial epoch of the integration. For convenience the evolution of the semi-major axes, eccentricities, the resonant angles (third row) and the Δωb,c are given for 500 and 105 years, respectively. The bottom row gives the orbital precession region, the sum of orbits for each integration output.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.