Stability of co-orbital motion in exoplanetary systems

Bálint Érdi, Zsolt Sándor

Research output: Contribution to journalArticle

34 Citations (Scopus)


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 L 4 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 L 4 in the elliptic restricted three-body problem is determined as a function of the mass parameter and eccentricity.

Original languageEnglish
Pages (from-to)113-121
Number of pages9
JournalCelestial Mechanics and Dynamical Astronomy
Issue number1-3
Publication statusPublished - Apr 1 2005



  • Co-orbital motion
  • Exoplanets
  • Nonlinear stability

ASJC Scopus subject areas

  • Modelling and Simulation
  • Mathematical Physics
  • Astronomy and Astrophysics
  • Space and Planetary Science
  • Computational Mathematics
  • Applied Mathematics

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