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Qualitative Dynamics of the Sun-Jupiter-Saturn System

Published online by Cambridge University Press:  12 April 2016

V. Szebehely
V. Szebehely*
Affiliation:
University of Texas, Austin, Texas

Abstract

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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.

Type
Part I. Planetary Theory and Analytical Methods
Information
International Astronomical Union Colloquium , Volume 41: Dynamics of Planets and Satellites and Theories of their Motion , 1978 , pp. 53 - 55
Copyright
Copyright © Reidel 1978

References

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