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A contour plot of the hours of daylight as a function of latitude and day of the year, using the most accurate models described in this article. Latitude 40° N (approximately New York City, Madrid and Beijing) is highlighted for reference[clarification needed]

The sunrise equation as follows can be used to derive the time of sunrise and sunset for any solar declination and latitude in terms of local solar time when sunrise and sunset actually occur:

where:

is the hour angle at either sunrise (when negative value is taken) or sunset (when positive value is taken);
is the latitude of the observer on the Earth;
is the sun declination.

Theory of the equationEdit

The Earth rotates at an angular velocity of 15°/hour. Therefore, the expression   gives the interval of time before and after local solar noon that sunrise or sunset will occur.[clarification needed]

The sign convention is typically that the observer latitude   is 0 at the equator, positive for the Northern Hemisphere and negative for the Southern Hemisphere, and the solar declination   is 0 at the vernal and autumnal equinoxes when the sun is exactly above the equator, positive during the Northern Hemisphere summer and negative during the Northern Hemisphere winter.

The expression above is always applicable for latitudes between the Arctic Circle and Antarctic Circle. North of the Arctic Circle or south of the Antarctic Circle, there is at least one day of the year with no sunrise or sunset. Formally, there is a sunrise or sunset when   during the Northern Hemisphere summer, and when   during the Northern Hemisphere winter. Out of these latitudes, it is either 24-hour daytime or 24-hour nighttime.

Generalized equationEdit

Also note that the equation above neglects the influence of atmospheric refraction (which lifts the solar disc by approximately 0.6° when it is on the horizon) and the non-zero angle subtended by the solar disc (about 0.5°). The times of the rising and the setting of the upper solar limb as given in astronomical almanacs correct for this by using the more general equation

 

with the altitude (a) of the center of the solar disc set to about −0.83° (or −50 arcminutes).

Complete calculation on EarthEdit

The generalized equation relies on a number of other variables which need to be calculated before it can itself be calculated. These equations have the solar-earth constants substituted with angular constants expressed in degrees.

Calculate current Julian dayEdit

 

where:

  is the number of days since Jan 1st, 2000 12:00.
  is the Julian date;
2451545.0 is the equivalent Julian year of Julian days for 2000, 1, 1.5, noon.
0.0008 is the fractional Julian Day for leap seconds and terrestrial time.
TT was set to 32.184 sec lagging TAI on 1 January 1958. By 1972, when the leap year was introduced, 10 sec were added. By 1 January 2017, 27 more seconds were added coming to a total of 69.184 sec. 0.0008=69.184 / 86400 without DUT1.

Mean solar noonEdit

 

where:

  is an approximation of mean solar time at   expressed as a Julian day with the day fraction.
  is the longitude west (west is negative, east is positive) of the observer on the Earth;

Solar mean anomalyEdit

 

where:

M is the solar mean anomaly used in a few of next equations.

Equation of the centerEdit

 

where:

C is the Equation of the center value needed to calculate lambda (see next equation).
1.9148 is the coefficient of the Equation of the Center for the planet the observer is on (in this case, Earth)

Ecliptic longitudeEdit

 

where:

λ is the ecliptic longitude.
102.9372 is a value for the argument of perihelion.

Solar transitEdit

 

where:

Jtransit is the Julian date for the local true solar transit (or solar noon).
2451545.0 is noon of the equivalent Julian year reference.
  is a simplified version of the equation of time. The coefficients are fractional day minutes.

Declination of the SunEdit

 

where:

  is the declination of the sun.
23.44° is Earth's maximum axial tilt toward the sun [1]

Hour angleEdit

This is the equation from above with corrections for astronomical refraction and solar disc diameter.

 

where:

ωo is the hour angle from the observer's zenith;
  is the north latitude of the observer (north is positive, south is negative) on the Earth.

For observations on a sea horizon needing an elevation-of-observer correction, add  , or   to the −0.83° in the numerator's sine term. This corrects for both apparent dip and terrestrial refraction. For example, for an observer at 10,000 feet, add (−115°/60°) or about −1.92° to −0.83°.

Calculate sunrise and sunsetEdit

 
 

where:

Jrise is the actual Julian date of sunrise;
Jset is the actual Julian date of sunset.

See alsoEdit

ReferencesEdit

External linksEdit