Abstract
Resonant asteroidal motion is investigated over 17 000 years in a three-dimensional elliptical model Sun-Jupiter-Asteroid averaged by Schubart’s method à la Poincarè. Orbits remain trapped in the resonance over this period. The various stability mechanisms are discussed. With respect to their behaviour of ω and \(\tilde \omega \), our resulting orbits reveal 5 distinct classes. These 5 classes can be described in Schubart’s topology for the planar problem. As compared to the planar case, eccentricities of orbits in the three-dimensional model vary more strongly. This is an important result for the problem of the delivery of meteorites.
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© 1983 D. Reidel Publishing Company, Dordrecht, Holland
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Scholl, H., Froeschle, C. (1983). Resonant Asteroidal Motion in the Kirkwood Gaps: A Three-Dimensional Study. In: Markellos, V.V., Kozai, Y. (eds) Dynamical Trapping and Evolution in the Solar System. Astrophysics and Space Science Library, vol 106. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7214-8_20
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DOI: https://doi.org/10.1007/978-94-009-7214-8_20
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-009-7216-2
Online ISBN: 978-94-009-7214-8
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