Sunrise equation

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

Formulation

It is formulated as:

:$\cos \omega_\circ = -\tan \phi \times \tan \delta$

where:
:$\omega_\circ$ is the solar hour angle at either sunrise (when negative value is taken) or sunset (when positive value is taken);
:$\phi$ is the latitude of the observer on the Earth;
:$\delta$ is the sun declination.

Principles

The Earth rotates at an angular velocity of 15°/hour. Therefore, the expression $\omega_\circ / \mathrm^\circ$, where $\omega_\circ$ is in degree, gives the interval of time in hours from sunrise to local solar noon or from local solar noon to sunset.

The sign convention is typically that the observer latitude $\phi$ is 0 at the equator, positive for the Northern Hemisphere and negative for the Southern Hemisphere, and the solar declination $\delta$ 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 $-90^\circ+\delta < \phi < 90^\circ - \delta$ during the Northern Hemisphere summer, and when $-90^\circ - \delta < \phi < 90^\circ + \delta$ during the Northern Hemisphere winter. For locations outside these latitudes, it is either 24-hour daytime or 24-hour nighttime.

Expressions for the solar hour angle

In the equation given at the beginning, the cosine function on the left side gives results in the range 1, 1 but the value of the expression on the right side is in the range \infty, \infty/math>. An applicable expression for $\omega_\circ$ in the format of Fortran 90 is as follows:

:

omegao = acos(max(min(-tan(delta*rpd)*tan(phi*rpd), 1.0), -1.0))*dpr

where omegao is $\omega_\circ$ in degree, delta is $\delta$ in degree, phi is $\phi$ in degree, rpd is equal to $\frac$, and dpr is equal to $\frac$.

The above expression gives results in degree in the range ^\circ, 180^\circ/math>. When $\omega_\circ=0^\circ$, it means it is polar night, or 0-hour daylight; when $\omega_\circ=180^\circ$, it means it is polar day, or 24-hour daylight.

Hemispheric relation

Suppose $\phi_$ is a given latitude in Northern Hemisphere, and $\omega_$ is the corresponding sunrise hour angle that has a negative value, and similarly, $\phi_$ is the same latitude but in Southern Hemisphere, which means $\phi_=-\phi_$, and $\omega_$ is the corresponding sunrise hour angle, then it is apparent that

:$\cos \omega_=-\cos \omega_=\cos (-180^\circ -\omega_)$,

which means

:$\omega_+\omega_=-180^$.

The above relation implies that on the same day, the lengths of daytime from sunrise to sunset at $\phi_$ and $\phi_$ sum to 24 hours if $\phi_=-\phi_$, and this also applies to regions where polar days and polar nights occur. This further suggests that the global average of length of daytime on any given day is 12 hours without considering the effect of atmospheric refraction.

Generalized equation

The equation above neglects the influence of atmospheric refraction (which lifts the solar disc — i.e. makes the solar disc appear higher in the sky — by approximately 0.6° when it is on the horizon) and the non-zero angle subtended by the solar disc — i.e. the apparent diameter of the sun — (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

:$\cos \omega_\circ = \dfrac$

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

The above general equation can be also used for any other solar altitude. The NOAA provides additional approximate expressions for refraction corrections at these other altitudes. There are also alternative formulations, such as a non-piecewise expression by G.G. Bennett used in the U.S. Naval Observatory's "Vector Astronomy Software".

Complete calculation on Earth

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 day

:$n = \lceil J_\text - 2451545.0 + 0.0008\rceil$
where:
:$n$ is the number of days since Jan 1st, 2000 12:00.
:$J_\text$ is the Julian date;
:2451545.0 is the equivalent Julian year of Julian days for Jan-01-2000, 12:00:00.
:0.0008 is the fractional Julian Day for leap seconds and terrestrial time (TT).
:TT was set to 32.184 sec lagging TAI on 1 January 1958. By 1972, when the leap second 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.
:The $\lceil \cdot \rceil$ operation rounds up to the next integer day number n.

Mean solar time

:$J^ = n - \dfrac$

where:

:$J^$ is an approximation of mean solar time at integer $n$ expressed as a Julian day with the day fraction.
:$l_\omega$ is the longitude (west is negative, east is positive) of the observer on the Earth;

Solar mean anomaly

:$M = (357.5291 + 0.98560028 \times J^) \bmod 360$

where:

:M is the solar mean anomaly used in the next three equations.

Equation of the center

:$C = 1.9148 \sin(M) + 0.0200 \sin(2 M) + 0.0003 \sin(3 M)$

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 longitude

:$\lambda = (M + C + 180 + 102.9372) \bmod 360$

where:

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

Solar transit

:$J_ = 2451545.0+J^ + 0.0053 \sin M - 0.0069 \sin \left( 2 \lambda \right)$

where:

:J_transit is the Julian date for the local true solar transit (or solar noon).
:2451545.0 is noon of the equivalent Julian year reference.
:$0.0053 \sin M - 0.0069 \sin \left( 2 \lambda \right)$ is a simplified version of the equation of time. The coefficients are fractional days.

Declination of the Sun

:$\sin \delta = \sin \lambda \times \sin 23.4397^\circ$

where:

:$\delta$ is the declination of the sun.
:23.4397° is Earth's maximum axial tilt toward the sun

Alternatively, the Sun's declination could be approximated as:

:$\delta = 23.45 * \sin((360 \times d / 365.25)^\circ)^\circ$

where:

: d is the number of days after the spring equinox (usually March 21st).

Hour angle

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

:$\cos \omega_\circ = \dfrac$

where:

:ω_o is the hour angle from the observer's meridian;
:$\phi$ 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 $-1.15^\circ\sqrt/60$, or $-2.076^\circ\sqrt/60$ to the −0.833° 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 −0.833°.The exact source of these numbers are hard to track down, bu
Notes on the Dip of the Horizon
provides a description yielding one less significant figure, with another page in the series providing -2.075.

Calculate sunrise and sunset

:$J_\text = J_\text - \dfrac$

:$J_\text = J_\text + \dfrac$

where:

:J_rise is the actual Julian date of sunrise;
:J_set is the actual Julian date of sunset.

Example of implementation in Python

#!/usr/bin/env python3

import logging
from datetime import datetime, timedelta, timezone, tzinfo
from math import acos, asin, ceil, cos, degrees, fmod, radians, sin, sqrt
from time import time

log = logging.getLogger()

def _ts2human(ts: int , float, debugtz: tzinfo , None) -> str:
return str(datetime.fromtimestamp(ts, debugtz))

def j2ts(j: float , int) -> float:
return (j - 2440587.5) * 86400

def ts2j(ts: float , int) -> float:
return ts / 86400.0 + 2440587.5

def _j2human(j: float , int, debugtz: tzinfo , None) -> str:
ts = j2ts(j)
return f" = "

def _deg2human(deg: float , int) -> str:
x = int(deg * 3600.0)
num = f"∠°"
rad = f"∠rad"
human = f"∠°′″"
return f" = = "

def calc(
current_timestamp: float,
f: float,
l_w: float,
elevation: float = 0.0,
*,
debugtz: tzinfo , None = None,
) -> tuple loat, float, None, tuple one, None, bool
log.debug(f"Latitude f = ")
log.debug(f"Longitude l_w = ")
log.debug(
f"Now ts = "
)

J_date = ts2j(current_timestamp)
log.debug(f"Julian date j_date = days")

# Julian day
# TODO: ceil ?
n = ceil(J_date - (2451545.0 + 0.0009) + 69.184 / 86400.0)
log.debug(f"Julian day n = days")

# Mean solar time
J_ = n + 0.0009 - l_w / 360.0
log.debug(f"Mean solar time J_ = days")

# Solar mean anomaly
# M_degrees = 357.5291 + 0.98560028 * J_ # Same, but looks ugly
M_degrees = fmod(357.5291 + 0.98560028 * J_, 360)
M_radians = radians(M_degrees)
log.debug(f"Solar mean anomaly M = ")

# Equation of the center
C_degrees = 1.9148 * sin(M_radians) + 0.02 * sin(2 * M_radians) + 0.0003 * sin(3 * M_radians)
# The difference for final program result is few milliseconds
# https://www.astrouw.edu.pl/~jskowron/pracownia/praca/sunspot_answerbook_expl/expl-4.html
# e = 0.01671
# C_degrees = \
# degrees(2 * e - (1 / 4) * e ** 3 + (5 / 96) * e ** 5) * sin(M_radians) \
# + degrees(5 / 4 * e ** 2 - (11 / 24) * e ** 4 + (17 / 192) * e ** 6) * sin(2 * M_radians) \
# + degrees(13 / 12 * e ** 3 - (43 / 64) * e ** 5) * sin(3 * M_radians) \
# + degrees((103 / 96) * e ** 4 - (451 / 480) * e ** 6) * sin(4 * M_radians) \
# + degrees((1097 / 960) * e ** 5) * sin(5 * M_radians) \
# + degrees((1223 / 960) * e ** 6) * sin(6 * M_radians)

log.debug(f"Equation of the center C = ")

# Ecliptic longitude
# L_degrees = M_degrees + C_degrees + 180.0 + 102.9372 # Same, but looks ugly
L_degrees = fmod(M_degrees + C_degrees + 180.0 + 102.9372, 360)
log.debug(f"Ecliptic longitude L = ")

Lambda_radians = radians(L_degrees)

# Solar transit (Julian date)
J_transit = (2451545.0 + J_ + 0.0053 * sin(M_radians) - 0.0069 * sin(2 * Lambda_radians))
log.debug(f"Solar transit time J_trans = ")

# Declination of the Sun
sin_d = sin(Lambda_radians) * sin(radians(23.4397))
# cos_d = sqrt(1-sin_d**2) # exactly the same precision, but 1.5 times slower
cos_d = cos(asin(sin_d))

# Hour angle
some_cos = (sin(radians(-0.833 - 2.076 * sqrt(elevation) / 60.0)) - sin(radians(f)) * sin_d) / (cos(radians(f)) * cos_d)
try:
w0_radians = acos(some_cos)
except ValueError:
return None, None, some_cos > 0.0
w0_degrees = degrees(w0_radians) # 0...180

log.debug(f"Hour angle w0 = ")

j_rise = J_transit - w0_degrees / 360
j_set = J_transit + w0_degrees / 360

log.debug(f"Sunrise j_rise = ")
log.debug(f"Sunset j_set = ")
log.debug(f"Day length {w0_degrees / (180 / 24):.3f} hours")

return j2ts(j_rise), j2ts(j_set), None

def main():
logging.basicConfig(level=logging.DEBUG)
latitude = 33.00801
longitude = 35.08794
elevation = 0
print(calc(time(), latitude, longitude, elevation, debugtz=timezone(timedelta(hours=3), "fake-zone")))

if __name__

"__main__":
main()

See also

* Day length
*Equation of time

References

External links

Sunrise, sunset, or sun position for any location – U.S. onlySunrise, sunset and day length for any location – WorldwideRise/Set/Transit/Twilight Data – U.S. onlyAstronomical Information CenterConverting Between Julian Dates and Gregorian Calendar DatesApproximate Solar CoordinatesAlgorithms for Computing Astronomical PhenomenaA Simple Expression for the Equation of TimeThe Equation of TimeEvaluating the Effectiveness of Current Atmospheric Refraction Models in Predicting Sunrise and Sunset Times

Equations
Time in astronomy
Dynamics of the Solar System
Articles with example Python (programming language) code