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Qualitative Dynamics of the Sun-Jupiter-Saturn System

  • V. Szebehely (a1)

Abstract

The stability of the three-body problem formed by the Sun, Jupiter and Saturn is investigated using surfaces of zero velocity. The results obtained with the models of the restricted and general problems of three bodies are compared with numerical integration. The system is found to be stable in the sense that Saturn will neither interrupt the (perturbed) binary orbit of Jupiter around the Sun, nor will it escape from the system. It is shown that the known classical triple stellar systems are “more stable” than the solar system, which in turn is “more stable” than the Earth-Moon system.

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Copyright

References

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Agekian, T.A., and Anosova, Z.P., (1967), Astronomical Zhurnal, 44, 1261.
Hill, G., (1878), Am. J. Math., 1, 5, 129, 245.
Nacozy, P., (1976), “On the Stability of the Solar System”, Astron. J., 81, 787.
Szebehely, V., (1967-a), Proc. U.S. Nat. Acad. Sc, 58, 60.
Szebehely, V., (1967-b), Theory of Orbits, Academic Press, New York, NY.
Szebehely, V., and McKenzie, R., (1977), “Stability of Planetary Systems with Bifurcation Theory”, Astron. J. 82, 79.

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