The shortest day of the year is the day of the winter solstice, usually December 21. It seems reasonable that the latest sunrise and earliest sunset would both occur on the shortest day. But it's not so; the earliest sunset is a couple of weeks earlier and the latest sunrise is a couple of weeks later. [Note 1] (The "notes" on this page contain additional explanation that can be skipped on first reading.)

What explains this peculiarity? Why doesn't the shortest day have the earliest sunset and latest sunrise?

The time of day when the sun reaches its highest point in the sky is
called *solar noon*. The period from one solar noon to the
next is called the *solar day*. One solar day is the time it
takes for the sun to return to its highest point in the sky.

The length of the solar day is not constant through the year. Near
the winter and summer solstices the solar day is *more* than 24
hours long, and near the spring and fall equinoxes it's *less* than
24 hours long. (Why so? We'll see shortly.) So solar noon
rarely occurs exactly at clock noon; it's sometimes before and sometimes
after. The critical point is this: *near the solstices,
solar noon occurs at a slightly later time each day* because the solar
day is more than 24 hours.

Now the time from solar noon to sunset doesn't change very much near the winter solstice [Note 2]. Therefore, since solar noon is a little later each day, sunset is also a little later each day. But if sunset is a little later each day, then the earliest sunset has already happened! Similarly, later solar noons at the solstice imply later sunrises, hence sunrise is getting later and the latest sunrise is yet to occur. [Notes 3, 4]

So the thing we need to understand is this: Why does the length of the solar day vary, and in particular why is it longer at the solstices?

There are two factors that change the length of the solar day. The
first is that the earth's axis is tilted with respect to its orbit around
the sun, and the second is that the earth's orbit is not a circle but an
ellipse. The first of these factors, called the *obliquity* of
the axis, has the larger effect and is the only one we examine
here [Note 5]. So let's study
the length of the solar day assuming that the earth orbits the sun in a
perfect circle.

Here's a summary: The length of the solar day is determined mostly
by the rotation of the earth on its axis, but is also affected a little bit
by the revolution of the earth around the sun. The rotation by itself
would make a constant-length solar day whether the axis was tilted or
not. The slight change caused by the revolution
would also be constant if the earth were not tilted, but because of the tilt it
is *not* constant; this slight change varies through the year
and makes the solar day longer near the solstices and shorter near the
equinoxes. Now for the details. [The explanation that follows
is based on a presentation by Andy Latto.]

At any instant, there is exactly one point on the earth's surface where the sun is directly overhead. To find it, draw a line from the center of the sun to the center of the earth and stand on the point where the line touches the earth's surface. At that point, and no other, the sun is exactly overhead. It is solar noon at that point and also everywhere else at the same longitude.

If the earth were motionless with respect to the sun, the
sun-directly-overhead point would always be in the same spot, no doubt
somewhere in Omaha, the tanning capital of the world [Note 6]. But the point moves, both because of the
rotation of the earth on its axis and because of the revolution of the
earth around the sun. When the point moves once around the earth, one
solar day has passed. When we say "once around the earth" we
care only about the *east-west* motion of the point---solar noon
recurs when the point traverses 360 degrees of longitude.
The *north-south* motion of the point doesn't matter to us since it
doesn't affect the length of a solar day.

First let's examine the effect of the earth's rotation. Imagine an untilted earth not revolving around the sun, just rotating, and it's obvious that the sun-directly-overhead point moves along the equator, once around per day. Now mentally tilt the earth's axis (like this) and you'll see that the point follows some other parallel of latitude, still once around per day. [Note 7] Since the point moves along a parallel of latitude, it moves in a purely east-west direction, in fact due west. If we measure speed in degrees of longitude per hour (not in miles per hour!) we realize that the speed of the point is constant, no matter what latitude it's at; it goes once around, 360 degrees, each day.

The bottom line is that the rotation of the earth causes the sun-directly-overhead point to move directly west, crossing lines of longitude at a constant rate. If this were the only factor to consider, the length of the solar day would be constant regardless of the tilt.

Now we have to add the effect of the earth's revolution around the
sun. Again, start by imagining the earth with untilted axis, this
time not rotating but just revolving around the sun. You'll see the
sun-directly-overhead point moving once around the earth each year.
And (take my word for this) the point moves eastward, so its motion is
*contrary* to the motion from the rotation---when added in, this
motion makes each solar day a little *longer* than it would be from
the rotation alone. (But just a very little, since the motion from
the revolution is so much slower.) If the earth were not tilted, the
motion due to revolution would be due east at constant rate, and would
lengthen each day equally throughout the year.

But the earth *is* tilted! So the earth's revolution around
the sun doesn't carry the sun-directly-overhead point along the
equator. It carries it around a great circle that's tilted with
respect to the equator. Imagine a band around the equator, and hold
it still while you tilt the earth. The band is now sometimes in the
northern hemisphere and sometimes in the southern, crossing the equator in
two places.

As the sun-directly-overhead point moves around this band, it is
*not* moving directly east. It moves generally east, but
sometimes it's travelling a little northeast and sometimes a little
southeast. It moves due east only at its most northerly and southerly
extent, which happens at the solstices.

So even though the overall speed of the point is constant,
the *eastward component* of the speed is not constant, and that's
what we care about: it's fastest when the point is moving due east
(at the solstices), and is smaller when the point is moving north or south
as well as east. The eastward speed is slowest when the point has the
largest northerly or southerly motion, that is, at the equinoxes, when the
point crosses the equator. [Note 8]

Hence this once-around-per-year motion of the point, which makes each day a little longer, has a different effect at different times of the year. At the solstices the motion is due east, so its eastward motion is fastest and lengthens the solar day more. That is, at the solstices, the solar day is longer than its average length. At the equinoxes, the point is moving northeast or southeast as much as it ever does, so the eastward component of its speed is at its slowest and has the least effect at making the day longer. That is, at the equinoxes, the solar day is a little shorter than average. And we're done.

One last comment: If you take a picture of the sun each day when
your clock says noon (*not* at local solar noon) the sun is not
always in the same place in the sky. It moves east and west because
of the variation in the length of the solar day, and it moves north and
south with the change of the seasons. The combination of these
motions traces out a figure-eight shape called
the *analemma* which you can
see pictured on some globes.

[1] The actual dates of earliest sunset and latest sunrise depend on latitude---near the equator, the earliest sunset occurs in November! Solstices and equinoxes happen at the same instant worldwide. back

[2] You might object to this: "The time
between solar noon and sunset isn't constant!" I hear you cry.
"It gets shorter in December and longer in July, making more or less
daylight!" Yes it does, but that change happens *very*
slowly near the solstices and can be ignored.

Think of it this way: There are two factors that change the time of sunset. The first is the change in the number of hours of daylight---we get fewer hours of daylight as we move towards December, which is reflected in earlier sunsets. The second factor is the difference between solar time and clock time, which we're explaining in this website (see Note 4). The first factor is the dominating factor through most of the year. Near the summer and winter solstices, though, the amount of daylight in the day is essentially constant, changing only a tiny amount from day to day, and the second factor comes into play. back

[3] We can apply the same reasoning to the summer
solstice to conclude that the *latest* sunset must *follow*
the summer solstice, and the *earliest* sunrise
must *precede* the summer solstice. Just remember that
*at either solstice, both sunrise and sunset are getting later* and
you can always tell where the earliest/latest sunrise/sunset occur.
back

[4] Here's another way to look at it: We don't
tell time using the solar day, because we want all days to have exactly the
same length. So we use clocks that run at a constant rate independent
of the sun, ticking off exactly 24 hours each day. These clocks
average out the variations in the solar day, making all days the same
length, and so don't agree with the solar day. But when we ask about
"earliest" sunset, of course we mean earliest according to the
constantly-running clocks! The difference between clock time and true
solar time creates the phenomenon we're investigating---if we used only
sundials to tell time, the earliest sunset and latest
sunrise *would* coincide with the winter solstice.
back

[5] The second factor that changes the length of the
solar day is called the *eccentricity* of the earth's orbit.
Not only does it have smaller effect than the obliquity, it works the other
way in summer---by itself, it would make the solar day *shorter*
than 24 hours at the summer solstice. At the winter solstice, the
obliquity and eccentricity work together to lengthen the solar day; at the
summer solstice, they oppose each other. Since the effect of the
obliquity is greater, the solar day is still longer at the summer
solstice. But because the total effect is less, there are a couple of
weeks between the earliest sunset and the winter solstice, but only several
days between the latest sunset and the summer solstice.
Go
here to see the individual contribution of each factor to the length of
the solar day. (The *equation of time*, the thing being
graphed, is just the difference between solar noon and clock noon.
Note that it's the slope of the equation of time, not its value, that's
important to this discussion.)

By the way, it's much easier to understand why the eccentricity changes the length of the solar day. You can find an explanation at any number of websites where the eccentricity is incorrectly trotted forward as the sole reason that the earliest sunset isn't the same day as the solstice! back

[6] This is a joke. The sun is never directly overhead in Omaha. The sun-directly-overhead point is confined to the tropics, that is, the belt between the Tropic of Cancer at 23.5 degrees north latitude and the Tropic of Heart Disease at 23.5 degrees south latitude. back

[7] Credit to Ken Driskell for the graphic. It's too bad that I don't have more visuals on this site; a picture is worth a thousand words and all that. If you'd like to help by creating graphics or animations to improve this page's explanations, winning undying honor and fame, please contact me. back

[8] The point doesn't move around the tilted circle at a truly constant speed, because the earth's orbit is not a perfect circle. The point moves slightly faster near perihelion (January) and slightly slower near aphelion (July). But the effect of this non-constant speed is less than the effect of the fact that the easterly speed varies depending on whether the point is going due east or northeast. In particular, the easterly component of the motion is at a near-maximum in July, because the fact that it is moving due east is more important than the fact that it's going a bit slower than usual. back

Copyright © 1997--2007 Larry Denenberg

Last modified 11/03/2007

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