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Solar time
Solar time
is a calculation of the passage of time based on the position of the Sun
Sun
in the sky. The fundamental unit of solar time is the day. Two types of solar time are apparent solar time (sundial time) and mean solar time (clock time).

Contents

1 Introduction 2 Apparent solar time 3 Mean solar time 4 History 5 See also 6 References 7 External links

Introduction A tall pole vertically fixed in the ground casts a shadow on any sunny day. At one moment during the day, the shadow will point exactly north or south (or disappear when and if the Sun
Sun
moves directly overhead). That instant is local apparent noon, or 12:00 local apparent time. About 24 hours later the shadow will again point north/south, the Sun seeming to have covered a 360-degree arc around the Earth's axis. When the Sun
Sun
has covered exactly 15 degrees (1/24 of a circle, both angles being measured in a plane perpendicular to the Earth's axis), local apparent time is 13:00 exactly; after 15 more degrees it will be 14:00 exactly. The problem is that in September the Sun
Sun
takes less time (as measured by an accurate clock) to make an apparent revolution than it does in December; 24 "hours" of solar time can be 21 seconds less or 29 seconds more than 24 hours of clock time. As explained in the equation of time article, this is due to the eccentricity of the Earth's orbit (i.e. the Earth's orbit
Earth's orbit
is not perfectly circular, meaning that the Earth- Sun
Sun
distance varies throughout the year), and the fact that the Earth's axis is not perpendicular to the plane of its orbit (the so-called obliquity of the ecliptic). The effect of this is that a clock running at a constant rate – e.g. completing the same number of pendulum swings in each hour – cannot follow the actual Sun; instead it follows an imaginary "mean Sun" that moves along the celestial equator at a constant rate that matches the real Sun's average rate over the year.[1] This is "mean solar time", which is still not perfectly constant from one century to the next but is close enough for most purposes. Currently a mean solar day is about 86,400.002 SI seconds.[2] The two kinds of solar time (apparent solar time and mean solar time) are among the three kinds of time reckoning that were employed by astronomers until the 1950s. (The third kind of traditional time reckoning is sidereal time, which is based on the apparent motions of stars other than the Sun.)[3] By the 1950s it had become clear that the Earth's rotation rate was not constant, so astronomers developed ephemeris time, a time scale based on the positions of solar system bodies in their orbits. Apparent solar time The apparent sun is the true sun as seen by an observer on Earth.[4] Apparent solar time or true solar time is based on the apparent motion of the actual Sun. It is based on the apparent solar day, the interval between two successive returns of the Sun
Sun
to the local meridian.[5][6] Solar time
Solar time
can be crudely measured by a sundial. The equivalent on other planets is termed local true solar time (LTST).[7][8] The length of a solar day varies through the year, and the accumulated effect produces seasonal deviations of up to 16 minutes from the mean. The effect has two main causes. First, Earth's orbit
Earth's orbit
is an ellipse, not a circle, so the Earth
Earth
moves faster when it is nearest the Sun (perihelion) and slower when it is farthest from the Sun
Sun
(aphelion) (see Kepler's laws of planetary motion). Second, due to Earth's axial tilt (known as the obliquity of the ecliptic), the Sun's annual motion is along a great circle (the ecliptic) that is tilted to Earth's celestial equator. When the Sun
Sun
crosses the equator at both equinoxes, the Sun's daily shift (relative to the background stars) is at an angle to the equator, so the projection of this shift onto the equator is less than its average for the year; when the Sun
Sun
is farthest from the equator at both solstices, the Sun's shift in position from one day to the next is parallel to the equator, so the projection onto the equator of this shift is larger than the average for the year (see tropical year). In June and December when the sun is farthest from the celestial equator a given shift along the ecliptic corresponds to a large shift at the equator. So apparent solar days are shorter in March and September than in June or December.

Length of apparent solar day (1998)[9]

Date Duration in mean solar time

February 11 24 hours

March 26 24 hours − 18.1 seconds

May 14 24 hours

June 19 24 hours + 13.1 seconds

July 25/26 24 hours

September 16 24 hours − 21.3 seconds

November 2/3 24 hours

December 22 24 hours + 29.9 seconds

These lengths will change slightly in a few years and significantly in thousands of years. Mean solar time Main article: Universal Time

The equation of time—above the axis a sundial will appear fast relative to a clock showing local mean time, and below the axis a sundial will appear slow.

Mean solar time is the hour angle of the mean Sun
Sun
plus 12 hours. This 12 hour offset comes from the decision to make each day start at midnight for civil purposes whereas the hour angle or the mean sun is measured from the zenith (noon).[10] Currently (2009) this is realized with the UT1 time scale, constructed mathematically from very long baseline interferometry observations of the diurnal motions of radio sources located in other galaxies, and other observations.[11][12] The duration of daylight varies during the year but the length of a mean solar day is nearly constant, unlike that of an apparent solar day.[13] An apparent solar day can be 20 seconds shorter or 30 seconds longer than a mean solar day.[9][14] Long or short days occur in succession, so the difference builds up until mean time is ahead of apparent time by about 14 minutes near February 6 and behind apparent time by about 16 minutes near November 3. The equation of time is this difference, which is cyclical and does not accumulate from year to year. Mean time follows the mean sun. Jean Meeus describes the mean sun as follows:

Consider a first fictitious Sun
Sun
travelling along the ecliptic with a constant speed and coinciding with the true sun at the perigee and apogee (when the Earth
Earth
is in perihelion and aphelion, respectively). Then consider a second fictitious Sun
Sun
travelling along the celestial equator at a constant speed and coinciding with the first fictitious Sun
Sun
at the equinoxes. This second fictitious sun is the mean Sun..."[15]

The length of the mean solar day is slowly increasing due to the tidal acceleration of the Moon
Moon
by the Earth
Earth
and the corresponding slowing of Earth's rotation by the Moon. History

Sun
Sun
and Moon, Nuremberg Chronicle, 1493

Many methods have been used to simulate mean solar time. The earliest were clepsydras or water clocks, used for almost four millennia from as early as the middle of the 2nd millennium BC until the early 2nd millennium. Before the middle of the 1st millennium BC, the water clocks were only adjusted to agree with the apparent solar day, thus were no better than the shadow cast by a gnomon (a vertical pole), except that they could be used at night. But it has long been known that the Sun
Sun
moves eastward relative to the fixed stars along the ecliptic. Since the middle of the first millennium BC the diurnal rotation of the fixed stars has been used to determine mean solar time, against which clocks were compared to determine their error rate. Babylonian astronomers knew of the equation of time and were correcting for it as well as the different rotation rate of the stars, sidereal time, to obtain a mean solar time much more accurate than their water clocks. This ideal mean solar time has been used ever since then to describe the motions of the planets, Moon, and Sun. Mechanical clocks did not achieve the accuracy of Earth's "star clock" until the beginning of the 20th century. Today's atomic clocks have a much more constant rate than the Earth, but its star clock is still used to determine mean solar time. Since sometime in the late 20th century, Earth's rotation has been defined relative to an ensemble of extra-galactic radio sources and then converted to mean solar time by an adopted ratio. The difference between this calculated mean solar time and Coordinated Universal Time
Time
(UTC) determines whether a leap second is needed. (The UTC time scale now runs on SI seconds, and the SI second, when adopted, was already a little shorter than the current value of the second of mean solar time.[16]) See also

Local mean time Meridian circle Earth
Earth
rotation Sidereal time Synodic day

References

^ Astronomical Almanac Online. (2011) Her Majesty's Nautical Almanac Office and the United States Naval Observatory. Glossary s.v. solar time. ^ Leap Seconds. (1999). Time
Time
Service Department, United States Naval Observatory. ^ For the three kinds of time, see (for example) the explanatory section in the almanac Connaissance des Temps for 1902, page 759. ^ Celestial Mechanics Chapter 6, J.B. Tatum, University of Victoria ^ Astronomical Almanac Online (2010). United States Naval Observatory. s.v. solar time, apparent; diurnal motion; apparent place. ^ Yallop, B. D. and Hohenkerk, C. Y. (August 1989). Solar Location Diagram (Astronomical Information Sheet No. 58). HM Nautical Almanac Office. ^ Allison, Michael; Schmunk, Robert (30 June 2015). "Technical Notes on Mars Solar Time
Time
as Adopted by the Mars24 Sunclock". Goddard Institute for Space
Space
Studies. National Aeronautics and Space Administration. Retrieved 8 October 2015.  ^ Allison, Michael; McEwen, Megan (2000). "A post-Pathfinder evaluation of areocentric solar coordinates with improved timing recipes for Mars seasonal/diurnal climate studies". Planetary and Space
Space
Science. 48 (2–3): 215. Bibcode:2000P&SS...48..215A. doi:10.1016/S0032-0633(99)00092-6.  ^ a b Jean Meeus (1997), Mathematical astronomy morsels (Richmond, VA: Willmann-Bell) 346. ISBN 0-943396-51-4. ^ http://www.idc-online.com/technical_references/pdfs/civil_engineering/Solar_Apparent_Time_and_Mean_Solar_Time.pdf ^ McCarthy, D. D. & Seidelmann, P. K. (2009). TIME From Earth Rotation to Atomic Physics. Weinheim: Wiley-VCH Verlag GmbH & Co. KGaA. ISBN 978-3-527-40780-4. pp. 68, 326. ^ Capitaine, N., Wallace, P. T., & McCarthy, D. D. (2003). "Expressions to implement the IAU 2000 definition of UT1", Astronomy and Astrophysics, vol.406 (2003), pp.1135-1149 (or in pdf form); and for some earlier definitions of UT1 see Aoki, S., H Kinoshita, H., Guinot, B., Kaplan, G. H., D D McCarthy, D. D., & Seidelmann, P. K. (1982) "The new definition of universal time", Astronomy and Astrophysics, vol.105 (1982), pp. 359-361. ^ For a discussion of the slight changes that affect the mean solar day, see the ΔT
ΔT
article. ^ "The duration of the true solar day". Pierpaolo Ricci. pierpaoloricci.it. (Italy) ^ Meeus, J. (1998). Astronomical Algorithms. 2nd ed. Richmond VA: Willmann-Bell. p. 183. ^ :(1) In "The Physical Basis of the Leap Second", by D D McCarthy, C Hackman and R A Nelson, in Astronomical Journal, vol.136 (2008), pages 1906-1908, it is stated (page 1908), that "the SI second is equivalent to an older measure of the second of UT1, which was too small to start with and further, as the duration of the UT1 second increases, the discrepancy widens." :(2) In the late 1950s, the cesium standard was used to measure both the current mean length of the second of mean solar time (UT2) (result: 9192631830 cycles) and also the second of ephemeris time (ET) (result:9192631770 ± 20 cycles), see "Time Scales", by L. Essen, in Metrologia, vol.4 (1968), pp.161-165, on p.162. As is well known, the 9192631770 figure was chosen for the SI second. L Essen in the same 1968 article (p.162) stated that this "seemed reasonable in view of the variations in UT2".

External links

Sunrise and Sunset and maximum Sun
Sun
altitude, all year long, anywhere Astrarium
Astrarium
Solar Tempometer: Apparent solar time in a digital display.

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