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Planetary perturbations of the Moon in ELP 2000

  • Part II: Motion of the Moon
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Abstract

A new solution for the planetary perturbations of the Moon is being built in the frame of ELP 2000, using Bretagnon's planetary theories, and achieved at the first order. It contains the two actions commonly distinguished: direct and indirect. The internal precision of computation is 2×10−6 arcsec. First-order planetary perturbations, in the direct case (Venus & Mars), have been compared to Standaert's solution. The major discrepancy reaches 70 cm in the longitude of Venus. Perturbations of the second order with respect to planetary masses, have been undertaken and illustrations are given. Finally, new values for the perigee and node motions are proposed.

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References

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Authors and Affiliations

  1. Service de Mécanique Céleste du Bureau des Longitudes, Equipe de Recherche associée au CNRS, Paris, France

    Jean Chapront & Michelle Chapront-Touze

Authors
  1. Jean Chapront
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  2. Michelle Chapront-Touze
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Additional information

Proceedings of the Conference on ‘Analytical Methods and Ephemerides: Theory and Observations of the Moon and Planets’. Facultés universitaires Notre Dame de la Paix, Namur, Belgium, 28–31 July, 1980.

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Chapront, J., Chapront-Touze, M. Planetary perturbations of the Moon in ELP 2000. Celestial Mechanics 26, 83–94 (1982). https://doi.org/10.1007/BF01233187

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  • DOI: https://doi.org/10.1007/BF01233187

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