This figure is much smaller than evection : the difference is accounted for by the fact that the ancient measurements were taken at times of eclipses, and the effect of the evection ( which subtracts under those conditions from the equation of the center ) was at that time unknown and overlooked . " For further information see also separate article Evection ."
12.
This figure is much smaller than evection : the difference is accounted for by the fact that the ancient measurements were taken at times of eclipses, and the effect of the evection ( which subtracts under those conditions from the equation of the center ) was at that time unknown and overlooked . " For further information see also separate article Evection ."
13.
This figure is much smaller than evection : the difference is accounted for by the fact that the ancient measurements were taken at times of eclipses, and the effect of the evection ( which subtracts under those conditions from the equation of the center ) was at that time unknown and overlooked . " For further information see also separate article Evection ."
14.
The Variation is the second-largest solar perturbation of the Moon's orbit after the Evection, and the third-largest inequality in the motion of the Moon altogether; ( the first and largest of the lunar inequalities is the equation of the centre, a result of the eccentricity & ndash; which is not an effect of solar perturbation ).
15.
The main visible effect ( in longitude ) of the variation of the Moon is that during the course of every month, at the octants of the Moon's phase that follow the syzygies ( i . e . halfway between the new or the full moon and the next-following quarter ), the Moon is about two thirds of a degree farther ahead than would be expected on the basis of its mean motion ( as modified by the equation of the centre and by the evection ).
16.
Evection causes the Moon's ecliptic longitude to vary by approximately & plusmn; 1.274?( degrees ), with a period of about 31.8 days . The evection in longitude is given by the expression + 4586.45 " \ sin ( 2D-l ), where D is the ( mean ) elongation, i . e . mean angular distance of the Moon from the Sun, and l is the moon's mean anomaly, i . e . mean angular distance of the moon from its perigee.
17.
Evection causes the Moon's ecliptic longitude to vary by approximately & plusmn; 1.274?( degrees ), with a period of about 31.8 days . The evection in longitude is given by the expression + 4586.45 " \ sin ( 2D-l ), where D is the ( mean ) elongation, i . e . mean angular distance of the Moon from the Sun, and l is the moon's mean anomaly, i . e . mean angular distance of the moon from its perigee.
