Stability of Co-Orbital Motion in Exoplanetary Systems

Details Stability of Co-Orbital Motion in Exoplanetary Systems Stability of Co-Orbital Motion in Exoplanetary Systems

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005cemda..92..113e&link_type=abstract

Celestial Mechanics and Dynamical Astronomy, Volume 92, Issue 1-3, pp. 113-121

Astronomy and Astrophysics

Astronomy

16

Co-Orbital Motion, Exoplanets, Nonlinear Stability

Scientific paper

The stability of co-orbital motions is investigated in such exoplanetary systems, where the only known giant planet either moves fully in the habitable zone, or leaves it for some part of its orbit. If the regions around the triangular Lagrangian points are stable, they are possible places for smaller Trojan-like planets. We have determined the nonlinear stability regions around the Lagrangian point L4 of nine exoplanetary systems in the model of the elliptic restricted three-body problem by using the method of the relative Lyapunov indicators. According to our results, all systems could possess small Trojan-like planets. Several features of the stability regions are also discussed. Finally, the size of the stability region around L4 in the elliptic restricted three-body problem is determined as a function of the mass parameter and eccentricity.

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