moon (m') would be in the opposite direction to the sun as seen from the earth, and would consequently be obscured by the shadow of the earth.
As, however, the moon's path is inclined to the ecliptic (§ 40), the latitudes of the sun and moon may differ by as much as 5°, either when they are in conjunction, i.e. when they have the same longitudes, or when they are
in opposition, i.e. when their longitudes differ by 180°, and they will then in either case be too far apart for an eclipse to occur. Whether then at any full or new moon an eclipse will occur or not, will depend primarily on the latitude of the moon at the time, and hence upon her position with respect to the nodes of her orbit (§ 40). If conjunction takes place when the sun and moon happen
to be near one of the nodes (n), as at s m in fig. 26, the sun and moon will be so close together that an eclipse will occur; but if it occurs at a considerable distance from a node, as at s' m', their centres are so far apart that no eclipse takes place.
Now the apparent diameter of either sun or moon is, as we have seen (§ 32), about 12°; consequently when their discs just touch, as in fig. 27, the distance between their centres is also about 12°. If then at conjunction the distance between their centres is less than this amount, an
