Abstract
In this chapter we investigate complexities of Moon’s motion [11], [49], [53]. The perturbing body is Sun itself; the magnitude of the perturbing force is thus relatively large. Here, we can no longer use the averaging principle (its error would skew some of our results by as much as a factor of two), thus, the time-dependent version of our formulas will be occasionally required. Traditionally, this problem has always been considered a benchmark for any new technique.
