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Stability of Co-Orbital Motion in Exoplanetary Systems

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Abstract

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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Authors and Affiliations

  1. Department of Astronomy, Eötvös University, Pázmány Péter s.1/A, H-1117, Budapest, Hungary

    Bálint Érdi & Zsolt Sándor

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  1. Bálint Érdi
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  2. Zsolt Sándor
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Correspondence to Bálint Érdi.

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Érdi, B., Sándor, Z. Stability of Co-Orbital Motion in Exoplanetary Systems. Celestial Mech Dyn Astr 92, 113–121 (2005). https://doi.org/10.1007/s10569-004-3114-5

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  • DOI: https://doi.org/10.1007/s10569-004-3114-5

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