# Relativistic Effects in the Motion of the Moon

• Bahram Mashhoon
• Dietmar S. Theiss
Conference paper
Part of the Lecture Notes in Physics book series (LNP, volume 562)

## Abstract

The main general relativistic effects in the motion of the Moon are briefly reviewed. The possibility of detection of the solar gravitomagnetic contributions to the mean motions of the lunar node and perigee is discussed.

## References

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It follows from a more complete treatment of the Newtonian problem that the mean motion of the lunar node can be characterized by a backward movement of frequency ω0N, which corresponds to a period of about 18.61 years. Similarly, the mean motion of the perigee can be characterized by a forward movement of frequency ω0P, which corresponds to a period of about 8.85 years. The theoretical expressions for N and P are rather complicated and depend on ω/Ω as well as the orbital eccentricities, etc. The first two terms of N and P in terms of ν =ω#x03A9;e given by $$N = 1 - 3v/8 - \cdot \cdot \cdot {\mathbf{ }}and{\mathbf{ }}P = 1 + 75v/8 + \cdot \cdot \cdot$$ . A detailed discussion of this subtle problem is given by D. Brouwer and G.M. Clemence, Celestial Mechanics (Academic Press, New York, 1961), Ch.12, especially pp. 320–323.Google Scholar