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.
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References
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For the motion of the Earth about the Sun, α≈ 7°0, ∈ ≈ 10-8 and ξ ≈ 2 x 10-5 based on the standard value of solar angular momentum [cf. C.W. Allen, Astrophysical Quantities, 3rd ed. (Athlone, London, 1973)]. The Fermi frame adopted in this paper is such that the nutation vanishes at τ = 0. This frame can be obtained from the results given in Ref. [11]; see, especially, p. 506.
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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.
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Mashhoon, B., Theiss, D.S. (2001). Relativistic Effects in the Motion of the Moon. In: Lämmerzahl, C., Everitt, C.W.F., Hehl, F.W. (eds) Gyros, Clocks, Interferometers...: Testing Relativistic Graviy in Space. Lecture Notes in Physics, vol 562. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-40988-2_15
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