Abstract
Coorbital configurations are special solutions of the three-body problem. In the restricted case (when the third body is a massless particle), it is well known that for small displacements from the triangular equilibrium points L 4 and L 5, the particle moves in a linearly stable 1:1 libration, provided the mass ratio is less than a critical value. There are two types of coorbital motion: “tadpole” orbits that enclose one of the triangular points and “horseshoe” orbits that enclose L 3, L 4 and L 5 (Dermott & Murray, 1981).
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Morais, M.H.M., Murray, C.D. (1999). Stability of Perturbed Coorbital Satellites. In: Steves, B.A., Roy, A.E. (eds) The Dynamics of Small Bodies in the Solar System. NATO ASI Series, vol 522. Springer, Dordrecht. https://doi.org/10.1007/978-94-015-9221-5_25
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DOI: https://doi.org/10.1007/978-94-015-9221-5_25
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