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27 returns to the same part of the ecliptic at the end of each period, and a recurrence of all eclipses within that interval must take place with little variation. This period is sometimes called the Moon’s cycle. The degree in which the Sun or Moon is eclipsed depends upon the Moon’s proximity to one of her nodes at the time of conjunction or opposition. If the Moon be upon the node at her change, or, in other words, it the centres of the Sun, Moon, and Earth be in the same line, and at the same time the Moon be in that part of her orbit nearest to the Earth, or in perigee , the eclipse will be total in that part of the Earth where the umbra, falls, and partial in those parts covered by the penumbra. But if the .'loon be in that part of her orbit most distant from the Earth, or in apogee , the umbra will not reach the Earth, and the eclipse will he annular , that is, the Moon will not totally obscure the Sun, but a ring of light will be left around her. Total and annular eclipses of the Sun are of very rare occurrence. It more often happens that the Moon at the time of conjunction is a few degrees on either side of her node, so that she is above or below the plane of the Earth’s orbit. In this case, the umbra will fall above or below the Earth, and the eclipse will be partial.—The same cause influences eclipses of the Moon; but owing to the large size of the Earth’s shadow, total eclipses of the Moon are more frequent than those of the Sun. The number of eclipses in any year cannot be more than seven, or fewer than two; the most usual number is four, two of each luminary. It must be remembered, however, that as an eclipse of the Moon is seen from any part of the Earth, whilst an eclipse of the Sun is only visible where the shadow falls, the former are much more frequently seen by a spectator at any one place than the latter. Besides occasioning the striking phenomena of