SOLAR TIME

time measured by the Earth's rotation relative to the Sun. Apparent solar time is that measured by direct observation of the Sun or by a sundial. Mean solar time, kept by most clocks and watches, is the solar time that would be measured by observation if the Sun traveled at a uniform apparent speed throughout the year rather than, as it actually does, at a slightly varying apparent speed that depends on the seasons. The difference between mean and apparent solar time is known as the equation of time. This is usually expressed as a correction, never exceeding about 16 minutes, which is added to or subtracted from one kind of solar time to determine the other. The real Sun and the imaginary mean Sun, from which mean solar time is measured, may be as much as 16 minutes apart because during the course of the year the apparent motion of the real Sun against the background of the stars alternately slows down and speeds up. There are two reasons for this. First, the Earth's orbit is not exactly circular, and the Earth moves in it at slightly different speeds at different seasons. Second, because the plane of the Earth's orbit is tilted relative to the plane of the Earth's Equator, the apparent daily course of the Sun is shifted by varying amounts during the year from a straight east-west direction, and the rate of change of the Sun's celestial longitude, from which solar time is derived, varies accordingly. Since 1972 the time in common use has been based on a combination of solar and atomic times; it is called Coordinated Universal Time (q.v.). Its second is the second of atomic time, while its epoch is kept by periodic adjustment within 0.9 second of mean solar time. See also Universal Time.