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Regions of Stability of Asteroids

Published online by Cambridge University Press:  12 April 2016

Victor Szebehely ,
Raimundo Vicente  and
John Lundberg
Victor Szebehely
Affiliation:
University of Texas, Austin
Raimundo Vicente
Affiliation:
University of Lisbon
John Lundberg
Affiliation:
University of Texas, Austin

Abstract

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Using Hill's modified stability criterium, regions of orbital elements are established for conditions of stability. The model of the three-dimensional restricted problem of three bodies is used with the Sun and Jupiter as the primaries. Four different cases are studied: direct and retrograde, outside and inside asteroidal orbits. The directions of the asteroidal orbits refer to the synodical reference frame and the positions refer to Jupiter's orbit. The orbital parameters of the asteroids are the semi-major axis (a), the eccentricity (e), and the inclination from Jupiter's orbital plane (i). The effects of the other orbital elements are not investigated in this paper. The argument of the perihelion and the longitude of the ascending node are fixed at Ω = ω = 90° and the time of perihelion passage is T = 0 for all orbits.

Type
Part III - Asteroids
Information
International Astronomical Union Colloquium , Volume 74: Dynamical Trapping and Evolution in the Solar System , 1983 , pp. 123 - 136
Copyright
Copyright © Reidel 1983

References

Hill, G. (1978), American Journal of Mathematics, Vol.1, p.5, p.129 and p. 245.CrossRefGoogle Scholar
Szebehely, V. (1967), “Theory of Orbits”, Academic Press, New York.Google Scholar
Szebehely, V. (1978), Proceedings of the National Academy of Sciences, Vol. 75, p.5743 CrossRefGoogle Scholar