Secondary resonances of co-orbital motions

Abstract

The size distribution of the stability region around the Lagrangian point L4 is investigated in the elliptic restricted three-body problem as the function of the mass parameter and the orbital eccentricity of the primaries. It is shown that there are minimum zones in the size distribution of the stability regions, and these zones are connected with secondary resonances between the frequencies of librational motions around L4. The results can be applied to hypothetical Trojan planets for predicting values of the mass parameter and the eccentricity for which such objects can be expected or their existence is less probable.

9 pages, 7 figures, accepted for publication in MNRAS

References in corpus (4)

• Observational Constraints on Trojans of Transiting Extrasolar Planets
• The 2:1 resonant exoplanetary system orbiting HD73526
• Could the 47 UMa Planetary System be a Second Solar System: predicting the Earth-like planets
• The Secular Evolution and Dynamical Architecture of the Neptunian Triplet Planetary System HD 69830

Cited by in corpus (4)

• Trojan resonant dynamics, stability, and chaotic diffusion, for parameters relevant to exoplanetary systems
• Reanalysis of radial velocity data from the resonant planetary system HD128311
• Frequencies and resonances around $L_4$ in the elliptic restricted three-body problem
• Modeling resonant trojan motion in planetary systems