224 sun positions — at 40°N the June solstice runs 14 h 51 min of daylight
Every pairing of 14 latitudes and 16 dates, worked out as a noon altitude, a length of day, sunrise and sunset in solar time, and a shadow length. Nothing is copied from a table: the day of the year gives the declination, and the declination meets the latitude. Refraction and the equation of time are left out, so these sunrise times sit several minutes — sometimes a quarter of an hour — away from clock time.
The declination comes from the date alone
The earth’s axis leans 23.44° out of its orbital plane, so the latitude that has the sun directly overhead at noon travels between −23.44° and +23.44° over a year. That latitude is the declination. The formula in common use is δ = 23.44° × sin(360° × (284 + N) ÷ 365), where N counts the days from 1 January. It reaches +23.44° at the June solstice, −23.44° at the December solstice, and crosses zero at the equinoxes — though this approximation puts the crossing about two days late.
Latitude and declination together fix the length of day
The hour angle H at which the sun meets the horizon follows from cos H = −tan(latitude) × tan(declination). The sky turns 15° an hour, so the day lasts 2H ÷ 15 hours, sunrise falls H ÷ 15 hours before noon and sunset the same amount after. When |cos H| passes 1 the arithmetic has not broken — that is the answer: above 1 the sun never rises (polar night), below −1 it never sets (midnight sun). Both show up in this table at 70°N in June and December, and those cells carry no clock times.
A shadow is the tangent of the altitude, read backwards
If the noon altitude is h, a pole 1 m tall casts 1 ÷ tan h metres of shadow. Measure the shadow instead and the altitude falls out, and from the altitude you can work back to a date or a latitude — that is how Eratosthenes measured the earth in antiquity. Shadows stretch fast as the sun drops: at 45° the shadow equals the height, at 30° it is 1.7 times as long, and at 5° more than eleven times.
What this leaves out
Sunrise here means the centre of the sun crossing the geometric horizon, an altitude of 0°. The usual convention adds refraction and the sun’s own radius and uses −0.833°, which makes the day 8 to 10 minutes longer at mid-latitudes. The clock is apparent solar time: to reach civil time you still have to add the equation of time (±16 minutes), the gap between your longitude and your time zone, and any summer time. The declination formula carries an error of up to 1.5°, leap years are not counted, so dates after February sit one day out, and neither the observer’s elevation nor hills and buildings on the horizon are in here.
A high sun is a strong sun
The higher the sun, the less air its light passes through, and the stronger the ultraviolet. As a rule of thumb, when your shadow is shorter than you are, the ultraviolet is near its peak for the day — how long skin lasts before it reddens depends on the index and the skin type.
See burn times by UV indexAt a glance
Length of day · Noon altitude
60°SJune solstice 6.56° · December solstice 53.44°
50°SJune solstice 16.56° · December solstice 63.44°
40°SJune solstice 26.56° · December solstice 73.44°
30°SJune solstice 36.56° · December solstice 83.44°
20°SJune solstice 46.56° · December solstice 86.56°
10°SJune solstice 56.56° · December solstice 76.56°
EquatorJune solstice 66.56° · December solstice 66.56°
10°NJune solstice 76.56° · December solstice 56.56°
20°NJune solstice 86.56° · December solstice 46.56°
30°NJune solstice 83.44° · December solstice 36.56°
40°NJune solstice 73.44° · December solstice 26.56°
50°NJune solstice 63.44° · December solstice 16.56°
60°NJune solstice 53.44° · December solstice 6.56°
70°NJune solstice 43.44° · December solstice -3.44°
Worth knowing
- Declination δ = 23.44° × sin(360° × (284 + N) ÷ 365), where N counts the days from 1 January.
- Noon altitude = 90° − |latitude − declination|; at the June solstice that is 90° − φ + 23.44° in the north.
- Length of day = 2H ÷ 15 hours with cos H = −tan(latitude) × tan(declination); beyond |cos H| = 1 lies polar day or night.
- Shadow = height ÷ tan(altitude). Times are apparent solar time, with refraction and the equation of time left out.
Times are apparent solar time, with noon set to 12:00 when the sun crosses the meridian.
Common questions
Q. How do I work out the length of a day?
Take cos H = −tan(latitude) × tan(declination) to get the hour angle H, then the day lasts 2H ÷ 15 hours. The declination comes from the date, so latitude and date are all you need. At the equinoxes the declination is near zero and every latitude gets close to twelve hours.
Q. Why does the equator always get twelve hours?
At latitude 0 the tangent of the latitude is 0, so cos H = 0 whatever the declination, which puts H at 90°. The seasons come and go but the day barely moves from twelve hours — add refraction and it runs a few minutes longer.
Q. Can I set my clock by these sunrise times?
Not directly. They are apparent solar time, so you still have to add the equation of time (±16 minutes), the gap between your longitude and your time zone, and summer time. Refraction is missing too, which makes the real sunrise 4 to 5 minutes earlier than shown.