First, the long axis (line of the apsides: perigee and apogee) of the Moon's elliptical orbit precesses eastward by one full cycle in just approximately 8.85 years. It is caused by the solar tide. This is the reason that an anomalistic month (the period of time that the Moon moves from the perigee to the apogee and to the perigee again) is longer than the sidereal month (the period of time when the Moon completes one revolution with respect to the fixed stars). This apsidal precession completes one rotation in the same time as the number of sidereal months exceeds the number of anomalistic months by exactly one, after about 3233 days (8.85 years).
Another precession is the turning of lunar orbit, the orientation of lunar orbit inclination. This motion determines the period of the lunar nodes; that is, the line along which the plane of the Moon's orbit and that of Earth's orbit intersect. This nodal period is about twice as long (about 18.6 years) as the apsidal precession period discussed above, and the direction of motion is Westward. This is the reason that a draconic month (the period of time that the Moon takes to return to the same node) is shorter than the sidereal month. After one nodal precession period, the number of draconic months exceeds the number of sidereal months by exactly one. This period is about 6793 days (18.60 years).
As a result of this nodal precession, the time for the Sun-Earth-Moon alignment to return to the same node, the eclipse year, is about 18.6377 days shorter than a sidereal year. The number of solar orbits during one turn of lunar orbit equals the period of orbit divided by this difference minus one.
Explanatory Supplement to the Astronomical Almanac, P.K. Seidelmann (ed.), US Naval Observatory / University Science Books (1992): pp. 114,115; p. 701
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