A periodic oscillation of the Earth’s pole about its mean position on the celestial sphere, due to the attractions of the Sun and Moon on the Earth’s equatorial bulge. It causes a small periodic variation in the positions of stars, and is superimposed on the much larger effect of precession. The main oscillation has an amplitude of about ±9″ and a period of 18.6 years, equal to the revolution period of the Moon’s nodes around the ecliptic. In addition there are many smaller oscillations, some with periods as small as a few days. Nutation is conventionally resolved into nutation in longitude and nutation in obliquity, which are respectively parallel and perpendicular to the ecliptic.