Many sources state that 12:00 noon is the high-point or mid-point of the sun's path across the sky.

However, for where I am, this is obviously wrong. In my own town the high point of the sun occurs at about 13:30 in the summer (because of DST), and 12:30 in the winter, but clearly not 12:00 noon.

Why, at different longitudes, is the high-point of the sun not at 12:00?

Thank you in advance.

  • $\begingroup$ What city are you in? If you don't want to use your actual city, any other at the same longitude in your time zone will work as well. $\endgroup$ – casey Nov 14 '15 at 3:01
  • $\begingroup$ The top answers seem to make it sound like the complexity of time zone shapes have to do with it... but regardless of that, it's just that sun sets later the further west you go. Such that the hour difference is spread around the timezone, so places in the eastern parts of a timezone are offset early (early sunrise, early solar noon, early sunset), and places in the western parts are offset to later sunrise\noon\sunset. Though Henning's answer does great to explain why there's other important things in play, such that it changes during the year. $\endgroup$ – JeopardyTempest Jul 14 '16 at 8:51
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    $\begingroup$ this is a realy good site for astronomical information timeanddate.com simply input where you are and get a lot of information. $\endgroup$ – trond hansen Jan 30 '18 at 8:21
  • $\begingroup$ Continuing trond hansen: including when solar noon/midnight are for your location throughout the year $\endgroup$ – JeopardyTempest Feb 6 '18 at 9:09

It's not a question of latitude but longitude and time zones.

Prior to the advent of railway transportation the time set on clocks varied from towns within close proximity because the clocks were set to noon when the Sun was at its highest in the sky. This was more apparent for towns east and west of each other (ie different longitudes).

When railway transportation was developed there was a need to standardize times so that train timetables could be developed and arrival and departure times would be accurate and consistent

This precipitated the development of time zones. Each time zone is approximately 15 degrees of longitude wide, but there are differences because of national/regional priorities. China which has a similar longitudinal extent as the contiguous states of the US has only one time zone, whereas there are four in the contiguous states of US.

Within a band of longitude the time is the same. In the time zones immediately east and west, the time is one hour more (east) and one hour less (west) - ignoring difference due to daily savings.

The reason for time zone being approximately 15 degrees of longitude wide is the rate of spin of the Earth is 15 degrees/hour (360 degrees every 24 hours).

You state that in your town, noon is either 12:30 or 13:30, depending on daylight saving time. The reason for noon occurring at half past the hour is due to the boundaries of the time zone where you live. Where I live, noon is approximately at quarter past the hour.

  • $\begingroup$ Well, I feel like a moron for not realizing that. Thank you! $\endgroup$ – Ian Paschal Nov 14 '15 at 20:10
  • $\begingroup$ It partly does rely on latitude, though. Consider the Arctic Circle on the solstices. $\endgroup$ – BarocliniCplusplus Nov 17 '15 at 15:54

Maybe a map will help visualise this a bit further:

enter image description here

Source: "Solar time vs standard time" by Stefano Maggiolo - How much is time wrong around the world?

As you can see, time zones are according to political boundaries, and this causes an offset from the official time to the solar time.

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    $\begingroup$ It doesn't actually matter how the boundaries of time zones are set. The very fact that they're zones and assign the same time to a range of longitudes means that solar noon can't correspond to civil noon at more than one longitude within the zone. Indeed, solar noon doesn't necessarily correspond to civil noon at any point within a timezone, for example because of daylight saving. $\endgroup$ – David Richerby Nov 14 '15 at 14:42
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    $\begingroup$ @DavidRicherby yes - exactly. Could have been a slightly more detailed answer! However, the political boundaries actually exacerbate the problem. Whereas in an ideal time zone allocation, you wouldn't have much offset from the solar noon, in other cases it can be quite large (e.g. China or Greenland) $\endgroup$ – Gimelist Nov 15 '15 at 23:28
  • $\begingroup$ This would make an awesome addition (i.e. edit) to Fred's answer. $\endgroup$ – kwinkunks Nov 16 '15 at 3:06
  • $\begingroup$ So why are so many of the time zones so deeply into the red? Even in many narrow zones the red completely dominates the blue... $\endgroup$ – curiousdannii Nov 16 '15 at 12:58
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    $\begingroup$ @curiousdannii: Being in the red part of the time zone has the same effect as having permanent DST -- it moves solar noon into the civil afternoon, which aligns better with human activity patterns in industrialized societies. Most people go to bed closer to civil midnight than they wake up, so being in the red part of a timezone helps avoid wasting daylight on parts of the civil day where most people are asleep anyway. $\endgroup$ – Henning Makholm Nov 16 '15 at 15:18

Time zones explain why you don't observe solar noon at 12:00 exactly, but not why the wall-clock time of solar noon varies with the seasons. In fact, even if you stay in place and don't observe DST, the time in the day where the sun is highest will vary throughout the year.

The fixed stars rotate around the celestial pole with a very constant speed (with extremely small and not completely predictable variations, less than milliseconds per day), so if you pick any fixed star and wait from it is highest in the sky to it is highest in the sky again, it will take 23 hours, 56 minutes, 4.1 second, each time.

The Sun moves in the sky more or less together with the fixed stars. It moves slowly among the fixed stars, at a speed of around one degree of arc per day, such that after a year it has traced out an entire great circle on the celestial sphere. This means that the time between two true noons (the times on two consecutive days where the Sun is highest on the sky) is on average about 4 minutes longer than the time between successive culminations of a fixed star.

However, because the Earth's orbit around the Sun is slightly eccentric, the speed of the sun relative to the fixed stars is not constant over the year. It moves quickest in early January and slowest in early July.

Additionally, the Sun doesn't move along the celestial equator -- it follows the ecliptic which is inclined by 23 degrees, so at some times during the year it will "waste" different portions of its daily motion among the fixed stars on north-south movement that doesn't contribute to the four-minute lengthening of the true-noon interval. On the other hand, near the solstices the Sun is nearer to the poles, and it takes less than one degree of east-west motion along the ecliptic to lengthen the day by 1/360 of 24 hours.

The combination of these two effects means that the apparent solar day (the time interval between two true noons) varies during the year between 23 hours 59 minutes 40 seconds and 24 hours 0 minutes 30 seconds. The cumulative effect of this is known as the equation of time, and can be as large as about half an hour -- that is, the time that passes between a true noon in early November and a true noon in early February will be about half an hour more than a multiple of 24 hours.

The zone time we use for ordinary timekeeping is adjusted such that the average difference over the year between true noon in Greenwich and 12:00 UTC is zero [*]. The second, which is the basic scientific unit of time, was originally defined as $\frac1{24\times 60\times 60}$ of the length of a mean solar day, but has since been redefined using atomic clocks. Once every several years a leap second is inserted into UTC to keep 12:00 UTC from drifting away from the averaged true noon time in Greenwich.

[*] Actually a slightly more complex process than simple averaging is used, which makes the outcome more precisely related to astronomical observables.

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    $\begingroup$ @njzk2: I think you must be misreading something. This answer does not claim that 23h56m is ever the time from highest sun to highest sun. $\endgroup$ – Henning Makholm Nov 15 '15 at 10:38
  • $\begingroup$ Oh, right. I missed the any fixed star part, I though you meant the sun. $\endgroup$ – njzk2 Nov 15 '15 at 17:56
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    $\begingroup$ "the time that passes between a true noon in early November and a true noon in early February will be about half an hour less than a multiple of 24 hours." It's half an hour more, not less. Where I am now, true solar noon today (Nov. 16) is 11:25 a.m. (standard time), and in February will be 11:55 a.m. $\endgroup$ – Ari Brodsky Nov 16 '15 at 14:41
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    $\begingroup$ @AriBrodsky: You're right, fixed. I'd even double-checked my reasoning, but thinking about timescales just seems to breed sign errors everywhere. $\endgroup$ – Henning Makholm Nov 16 '15 at 15:08

Henning Makholm's answer is excellent but omits the elegant definition of the mean Sun, which is what the clock at the Prime Meridian attempts to match:

Consider a first fictitious Sun travelling along the ecliptic with a constant speed and coinciding with the true sun at the perigee and apogee (when the Earth is in perihelion and aphelion, respectively).

This removes the variation due to the orbit's eccentricity. The orbit is symmetric about the line through perihelion and aphelion, so this makes the average offset zero.

Then consider a second fictitious Sun travelling along the celestial equator at a constant speed and coinciding with the first fictitious Sun at the equinoxes. This second fictitious sun is the mean Sun...

This second step removes the variation due to axial tilt; again, the matching-points are chosen for symmetry.

J. Meeus (1998). Astronomical Algorithms. 2nd ed. Richmond VA: Willmann-Bell. p. 183.

  • $\begingroup$ +1, nice point. I hadn't realized that this definition actually produces exact zero average equation of time. $\endgroup$ – Henning Makholm Nov 16 '15 at 13:48
  • $\begingroup$ Oops, the equinoxes are the only points where the two fictitious Suns can coincide! $\endgroup$ – Anton Sherwood Dec 8 '16 at 6:48

Cannot add to the excellent Time Zone, Daylight Savings, and Equation of Time (Mean Sun) explanations here, but I do want to mention something about the original question by Ian Paschal. It appears to be assumed that the high-point (culmination) and mid-point (transit) are the same, or that the point of highest altitude occurs on the celestial meridian. Though true for the stars, for other celestial bodies these are different. As D.A. Pio puts it in Longitude from Moon Culminations (Royal Astronomical Society, Vol. 59, 1899; p. 513):

The author reminds the reader that only the fixed stars culminate really in the meridian. The Sun, the Moon, and all the planets culminate out of the meridian.

Jürgen Giesen gives a mathematical analysis of it here:


The difference is quite small for the sun, up to 18 seconds at mid-latitudes (I believe this is ignored in celestial navigation), but it can be more than 6 minutes in the case of the moon.

Also related (tangentially) to Paschal's question, back before time zones and widely-available accurate timepieces, there were specialized sundials called noon-marks whose sole purpose was to indicate the Local Apparent Noon (LAN).


Well, Sun was there before people and any concept of time. When people emerged, they naturally considered night as period when there is no Sun and Day where there was Sun on the sky.

When time was invented for the first time (ancient civilisations), most likely 12 was the time when the Sun was the highest on the sky. Then people became smarter and introduced different timezones in order to standardise the concept of time and this caused some deviations.

Then people thought they will be more productive (making more money) if there introduce the concept of Winter and Summer time what introduced further time deviations.

Therefore you do not see it anymore point 12.


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