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The '''astronomical unit''' (abbreviated variously as '''AU''', '''au''', '''a.u.''' or '''ua''') is a unit of [[length]] roughly equal to the mean distance of the [[Earth]] from the [[Sun]]. The currently accepted value of the AU is 1.49597870691 x 10<sup>11</sup> (± 3) meters (m), which is approximately 150 million kilometers (km) or 93 million miles. This unit has been particularly useful for calculating the distances of [[planet]]s and other objects in the [[Solar System]], relative to the Earth's distance from the Sun.

== Defining the distance ==

The astronomical unit was originally defined as the [[length]] of the [[semimajor axis]]<ref>The semimajor axis of an elliptical orbit is half the length of the major axis of the ellipse.</ref> of the Earth's elliptical orbit around the Sun. In 1976, the International Astronomical Union revised the definition of the AU for greater precision, defining it as the distance from the center of the Sun at which a [[test particle|particle]] of negligible [[mass]], in an unperturbed circular orbit, would have an [[orbital period]] of 365.2568983 days (one [[Gaussian year]]). More accurately, it is the distance at which the heliocentric [[gravitational constant]] (the product ''GM''<sub>☉</sub>) is equal to (0.017 202 093 95)² AU³/d².

== Abbreviations used ==

The abbreviation "ua" is recommended by the [[Bureau International des Poids et Mesures]]<ref>[http://www.bipm.org/en/si/si_brochure/chapter4/table7.html Non-SI units accepted for use with the SI, and units based on fundamental constants] ''Bureau International des Poids et Mesures''. Retrieved December 4, 2007.</ref>, but in the [[United States]] and other [[anglophone]] countries the reverse lettering (AU or au) is more common. The [[International Astronomical Union]] recommends "au"<ref>[http://www.iau.org/Units.234.0.html Recommendations concerning Units.] ''International Astronomical Union.'' Retrieved December 4, 2007.</ref>, and the [[international standard]] [[ISO 31-1]] uses "AU."

==History==

[[Aristarchus of Samos]] estimated the distance to the Sun to be about 20 times the distance to the Moon, whereas the true ratio is about 390. His estimate was based on the angle between the half moon and the sun, which he calculated to be 87°.

According to [[Eusebius of Caesarea]] in the ''[[Praeparatio Evangelica]]'', [[Eratosthenes]] found the distance to the sun to be "σταδιων μυριαδας τετρακοσιας και οκτωκισμυριας" (literally "of stadia myriads 400 and 80000"). This has been translated either as 4,080,000 [[Stadia (method)|stadia]] (1903 translation by [[Edwin Hamilton Gifford]]), or as 804,000,000 stadia (edition of [[Édouard des Places]], dated 1974-1991). Using the Greek stadium of 185 to 190 meters, the former translation comes to a far-too-low 755,000 km, whereas the second translation comes to 148.7 to 152.8 million km (accurate within two percent).

At the time the AU was introduced, its actual value was very poorly known, but planetary distances in terms of AU could be determined from heliocentric geometry and [[Kepler's laws of planetary motion]]. The value of the AU was first estimated by [[Jean Richer]] and [[Giovanni Domenico Cassini]] in 1672. By measuring the [[parallax]] of [[Mars (planet)|Mars]] from two locations on the Earth, they arrived at a figure of about 140 million kilometers.

A somewhat more accurate estimate can be obtained by observing the [[transit of Venus]]. This method was devised by [[James Gregory (astronomer and mathematician)|James Gregory]] and published in his ''[[Optica Promata]]''. It was strongly advocated by [[Edmond Halley]] and was applied to the transits of Venus observed in 1761 and 1769, and then again in 1874 and 1882.

Another method involved determining the constant of [[aberration of light|aberration]], and [[Simon Newcomb]] gave great weight to this method when deriving his widely accepted value of 8.80" for the [[solar parallax]] (close to the modern value of 8.794148").

The discovery of the [[near-Earth asteroid]] [[433 Eros]] and its passage near the Earth in 1900&ndash;1901 allowed a considerable improvement in parallax measurement. More recently very precise measurements have been carried out by [[radar]] and by [[telemetry]] from [[space probe]]s.

While the value of the astronomical unit is now known to great precision, the value of the mass of the Sun is not, because of uncertainty in the value of the [[gravitational constant]]. Because the gravitational constant is known to only five or six significant digits while the positions of the planets are known to 11 or 12 digits, calculations in celestial mechanics are typically performed in solar masses and astronomical units rather than in kilograms and kilometers. This approach makes all results dependent on the gravitational constant. A conversion to [[SI]] units would separate the results from the gravitational constant, at the cost of introducing additional uncertainty by assigning a specific value to that unknown constant.

== Examples ==

The distances are approximate mean distances. It has to be taken into consideration that the distances between [[astronomical object|celestial bodies]] change in [[time]] due to their [[orbit]]s and other factors.

* The [[Earth]] is 1.00 ± 0.02 AU from the [[Sun]].
* The [[Moon]] is 0.0026 ± 0.0001 AU from the Earth.
* [[Mars (planet)|Mars]] is 1.52 ± 0.14 AU from the Sun.
* [[Jupiter]] is 5.20 ± 0.05 AU from the Sun.
* [[Pluto]] is 39.5 ± 9.8 AU from the Sun.
* [[90377 Sedna]]'s orbit ranges between 76 and 942 AU from the Sun; Sedna is currently ([[as of 2006]]) about 90 AU from the Sun.
* As of August 2006, [[Voyager 1]] is 100 AU from the Sun, the furthest of any man-made object.
* [[Proxima Centauri]] (the nearest [[star]]) is ~268 000 AU away from the Sun.
* The mean diameter of [[Betelgeuse]] is 2.57 AU.
* The distance from the Sun to the center of the [[Milky Way]] is approximately 1.7×10<sup>9</sup> AU.
* The [[Earth]] is actually 147,104,753 km away from the [[Sun]] on December 29 and 152,091,803 km away from the Sun on June 30.

Some conversion factors:
* 1 AU = 149,597,870.691 ± 0.030 km ≈ 92,955,807 miles ≈ 8.317 [[light-year|light minutes]] ≈ 499 [[light-second]]s
* 1 [[light-second]] ≈ 0.002 AU
* 1 [[gigameter]] ≈ 0.007 AU
* 1 [[light-minute]] ≈ 0.120 AU
* 1 [[microparsec]] ≈ 0.206 AU
* 1 [[terameter]] ≈ 6.685 AU
* 1 [[light-hour]] ≈ 7.214 AU
* 1 [[light-day]] ≈ 173.263 AU
* 1 [[milliparsec]] ≈ 206.265 AU
* 1 [[light-week]] ≈ 1212.84 AU
* 1 [[light-month]] ≈ 5197.9 AU
* 1 [[light-year]] ≈ 63 241 AU
* 1 [[parsec]] ≈ 206 265 AU

== See also ==

* [[Earth]]
* [[Sun]]

== Notes ==
<references/>

== References ==

* Fenna, Donald. 2002. ''A Dictionary of Weights, Measures, and Units''. Oxford: Oxford University Press. ISBN 0198605226
* Maran, Stephen P. 2005. ''Astronomy for Dummies''. 2nd ed. Hoboken, NJ: Wiley. ISBN 0764584650
* McCarthy, D.D., ed. July 1996. IERS Technical Note 21. ''IERS Conventions''. Paris: Observatoire de Paris.
* Pennycuick, C.J. 1988. ''Conversion Factors: S. I. Units and Many Others''. Chicago: University of Chicago Press. ISBN 0226655075
* Standish, E. Myles. 1995. "Report of the IAU WGAS Sub-group on Numerical Standards." In ''Highlights of Astronomy'', I. Appenzeller, ed. Dordrecht: Kluwer Academic Publishers. (Tables from this report are available at [http://ssd.jpl.nasa.gov/?constants Astrodynamic Constants], a NASA Web site. Retrieved December 4, 2007.)

== External links ==

* [http://physics.nist.gov/cuu/Units/outside.html Units outside the SI] ''National Institute of Standards and Technology''. Retrieved December 4, 2007.
* [http://www.iau.org/Units.234.0.html Recommendations concerning Units] ''International Astronomical Union''. Retrieved December 4, 2007.
* [http://home.comcast.net/~pdnoerd/SMassLoss.pdf Solar Mass Loss, the Astronomical Unit, and the Scale of the Solar System] (A discussion of the relation between the AU and other quantities.) Retrieved December 4, 2007.

[[Category:Physical sciences]]
[[Category:Astronomy]]

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