# equation of time

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## equation of time:

see solar time**solar time,**

time defined by the position of the sun. The solar day is the time it takes for the sun to return to the same meridian in the sky. Local solar time is measured by a sundial.

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## equation of time

The correction that must be applied to apparent solar time to obtain mean solar time, i.e. it is the difference in time as measured by a sundial and by a clock. The equation of time varies through the year; it has two maxima and two minima and is zero on four dates: April 15/16, June 14/15, Sept. 1/2, and Dec. 25/26. A positive value indicates that apparent time is ahead of mean time; the greatest positive value, which can be over 16 minutes, occurs in early Nov.; the greatest negative value, over 14 minutes, occurs in mid-Feb. The curve is the sum of two components, each reflecting a nonuniformity in the apparent motion of the Sun: one component arises from the ellipticity of the Earth's orbit, the other from the inclination of the ecliptic to the celestial equator (see mean Sun).*The Great Soviet Encyclopedia*(1979). It might be outdated or ideologically biased.

## Equation of Time

the difference between mean solar time and apparent solar time, equal to the difference between the right ascensions of the true sun and the mean sun. The equation of time is often defined as the difference between apparent time and mean time; in this case, the equation has the opposite sign, a fact that must be borne in mind when reference books are used.

The equation of time varies continuously. The variation is due to the fact that the passage of apparent solar time, as measured by the hour angle of the true sun, is nonuniform because of the nonuniformity of the earth’s orbital motion and the inclination of the ecliptic to the equator. Therefore, the equation of time is obtained by adding two waves of approximately sinusoidal shape and nearly equal amplitude (see Figure 1). One of the waves has an annual period; the other, a semiannual period. The equation of time is equal to zero four times a year—around Apr. 16, June 14, Sept. 1, and Dec. 25. Four times a year it attains the following largest absolute values: +14.3 min (around Feb. 12), –3.8 min (around May 15), +6.4 min (around July 27), and –16.4 min (around Nov. 4).

We can find the local mean solar time by using the equation of time if we know the apparent solar time, as determined from observations of the sun with, for example, a sundial. In this case, we use the following formula:

*m* = *m*_{0} + η

where *m* is the mean time, *m*_{0} is the apparent time, and η in is the equation of time.

Values of the equation of time for each day are given in astronomical almanacs and calendars. (*See*.)