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Libration of the Moon: shape of the Earth and motion of the ecliptic plane

Published online by Cambridge University Press:  04 August 2017

M. Moons
M. Moons*
Affiliation:
Dept. of Mathematics, Facultés Universitaires N.D. de la Paix, B-5000 Namur, Belgium

Abstract

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Very accurate theories of the libration of the Moon have been recently built by Migus (1980), Eckhardt (1981, 1982) and Moons (1982, 1984). All of them take into account the perturbation due to the Earth and the Sun on the motion of a rigid Moon about its center of mass. Additional perturbations (influence of the planets, shape of the Earth, elasticity of the Moon, …) are also often included.

We present here the perturbations due to the shape of the Earth and the motion of the ecliptic plane on our theory which already contains planetary perturbations. This theory is completely analytical with respect to the harmonic coefficients of the lunar gravity field which is expanded in spherical harmonics up to the fourth order. The ELP 2000 solution (Chapront and Chapront-Touzé, 1983) supplies us with the motion of the center of mass of the Moon.

Type
Motions of Natural Bodies in the Solar System
Information
Symposium - International Astronomical Union , Volume 114: Relativity in Celestial Mechanics and Astrometry , 1986 , pp. 141 - 144
Copyright
Copyright © Reidel 1986 

References

Chapront, J., Chapront-Touzé, M. (1983). Astron. Astrophys. 124, 50–62.Google Scholar
Eckhardt, D.H. (1981). The Moon and the Planets 25, 3–49.Google Scholar
Eckhardt, D.H. (1982). In “High-Precision Earth Rotation and Earth-Moon Dynamics”, Ed. Calame, O., 193–198.Google Scholar
Migus, A. (1980). The Moon and the Planets 23, 391–427.CrossRefGoogle Scholar
Moons, M. (1982). The Moon and the Planets 27, 257–284.Google Scholar
Moons, M. (1984). Celestial Mechanics 34, 263–273.Google Scholar