Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-26T03:20:57.075Z Has data issue: false hasContentIssue false
  • English
  • Français

Hori Auxiliary System for Mimas-Tethys

Published online by Cambridge University Press:  07 August 2017

Wagner Sessin
Wagner Sessin*
Affiliation:
Depto. de Mecânica do Vôo e Orbital Instituto Tecnológico de Aeronáutica 12225, São José dos Campos, SP, Brasil

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

It is considered the problem of two natural satellites around a spheric planet. Only gravitational forces act on the system. The satellites move in a central field disturbed by the mutual atraction between them. The disturbing function is developed in power series of the small parameter (ratio of mass of satellites and planet), of the eccentricities and inclinations (assumed small) of the satellites' orbits. The mean motions are supposed to be commesurable in the ratio 2:1. It is, also, assumed that the critical angles are of inclination type. The critical angles of eccentricity type circulates and may be eliminate as fast variables like the short-periodic terms. The hamiltonian is truncated up to the second order in the inclinations.

Type
Part IV - Planetary Satellites
Information
Symposium - International Astronomical Union , Volume 152: Chaos, Resonance and Collective Dynamical Phenomena in the Solar System , 1992 , pp. 223 - 226
Copyright
Copyright © Kluwer 1992 

References

Greenberg, R.:1973, Mon. Not. R. astr. Soc. 165, 305.CrossRefGoogle Scholar
Jefferys, W.H.:1966, Astron. J. 71, 306.CrossRefGoogle Scholar
Lemaître, A.:1984, Celest. Mech. 32, 109.CrossRefGoogle Scholar
Sessin, W. and Ferraz-Mello, S.:1984, Celest. Mech. 32, 307.CrossRefGoogle Scholar