By J. Kovalevsky (auth.), Vassilis V. Markellos, Yoshihide Kozai (eds.)
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Extra resources for Dynamical Trapping and Evolution in the Solar System: Proceedings of the 74th Colloquium of the International Astronomical Union Held in Gerakini, Chalkidiki, Greece, 30 August – 2 September, 1982
The evolution of the Laplace commensurability and of the periods of the satellites is also of great current interest. The studies by 51 v. V. Markellos and Y. ), Dynamical Trapping and Evolution in the Solar System, 51-59. © 1983 by D. Reidel Publilhing Company. 1. H. LIESKE 52 Peale et al (1979, 1980), Greenberg (1980), Yoder (1979), and Yoder and Peale (1981) all present scenarios which would benefit greatly from analyses which can only effectively be done by employing the old data over a long time-span.
H. LIESKE Figure 1.
1). For describing an orientation of a third coordinate system relative to the second one we use Euler's angles: ~, S, ~ in 1-2-1 sequence (Markley 1978). Next we assume that the third rigid body-satellite- is axially symmetric and is located at the triangular L4 libration point. The Lagrange function has the form L = 1 "2 T w (1) Iw - V where T w W. l w. (~,8, ~, ~, l e, ~), 27 v. © V. Markellos and Y. ), Dyruzmical Trapping and Evolution in the Solar System, 27-35. 1983 by D. Reidel Publishing Company.