SI units  

149.60×10 ^{6} km  149.60×10 ^{9} m 
Astronomical units  
4.8481 × 10^{−6} pc  15.813×10 ^{−6} ly 
US customary / Imperial units  
92.956×10 ^{6} mi  490.81×10 ^{9} ft 
An astronomical unit (abbreviated as AU, au, a.u., or sometimes ua) is a unit of length equal to about 149,597,871 kilometres^{[1]} (92,955,807 miles). It is defined by the International Astronomical Union, and is defined as the mean distance between the Earth and the Sun over one Earth orbit.
The symbol ua is recommended by the International Bureau of Weights and Measures,^{[2]} but au is more common in Anglosphere countries. The International Astronomical Union recommends au,^{[3]} while international standard ISO 311 uses AU. In general, capital letters are only used for the symbols of units which are named after individual scientists, while au or a.u. can also mean atomic unit or even arbitrary unit; however, the use of AU to refer to the astronomical unit is widespread.^{[4]} The astronomical constant whose value is one astronomical unit is referred to as unit distance and given the symbol A.
Contents 
Originally, the AU was defined as the length of the semimajor axis 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 that length for which the Gaussian gravitational constant (k) takes the value 0.017 202 098 95 when the units of measurement are the astronomical units of length, mass and time.^{[5]} An equivalent definition is the radius of an unperturbed circular Newtonian orbit about the Sun of a particle having infinitesimal mass, moving with a angular frequency of 0.017 202 098 95 radians per day,^{[6]} or that length for which the heliocentric gravitational constant (the product GM_{☉}) is equal to (0.017 202 098 95)^{2} AU^{3}/d^{2}. It is approximately equal to the mean Earth–Sun distance.
Very precise measurements of the relative positions of the inner planets can be made by radar and by telemetry from space probes. As with all radar measurements, these rely on measuring the time taken for light to be reflected from an object. These measured positions are then compared with those calculated by the laws of celestial mechanics: the calculated positions are often referred to as an ephemeris, and are usually calculated in astronomical units. The comparison gives the speed of light in astronomical units, which is 173.144 632 6847(69) AU/d (TDB).^{[7]} As the speed of light in metres per second (c_{SI}) is fixed in the International System of Units, this measurement of the speed of light in AU/d (c_{AU}) also determines the value of the astronomical unit in metres (A):
The International Astronomical Union (IAU) currently accepted best estimate (2009) of the value of the astronomical unit in metres is A = 149 597 870 700(3) m, based on a comparison of JPL and IAA–RAS ephemerides.^{[8]}^{[9]}^{[10]}
By definition, the astronomical unit is dependent on the heliocentric gravitational constant, that is the product of the gravitational constant G and the solar mass M_{☉}. Neither G nor M_{☉} can be measured to high accuracy in SI units, but the value of their product is known very precisely from observing the relative positions of planets (Kepler's Third Law expressed in terms of Newtonian gravitation). Only the product is required to calculate planetary positions for an ephemeris, which explains why ephemerides are calculated in astronomical units and not in SI units.
The calculation of ephemerides also requires a consideration of the effects of general relativity. In particular, time intervals measured on the surface of the Earth (terrestrial time, TT) are not constant when compared to the motions of the planets: the terrestrial second (TT) appears to be longer in Northern Hemisphere winter and shorter in Northern Hemisphere summer when compared to the "planetary second" (conventionally measured in barycentric dynamical time, TDB). This is because the distance between the Earth and the Sun is not fixed (it varies between 0.983 289 8912 AU and 1.016 710 3335 AU) and, when the Earth is closer to the Sun (perihelion), the Sun's gravitational field is stronger and the Earth is moving faster along its orbital path. As the metre is defined in terms of the second, and the speed of light is constant for all observers, the terrestrial metre appears to change in length compared to the "planetary metre" on a periodic basis.
The metre is defined to be a unit of proper length, but the SI definition does not specify the metric tensor to be used in determining it. Indeed, the International Committee for Weights and Measures (CIPM) notes that "its definition applies only within a spatial extent sufficiently small that the effects of the nonuniformity of the gravitational field can be ignored."^{[11]} As such, the metre is undefined for the purposes of measuring distances within the solar system. The 1976 definition of the astronomical unit is incomplete, in particular because it does not specify the frame of reference in which time is to be measured, but has proved practical for the calculation of ephemerides: a fuller definition that is consistent with general relativity has been proposed.^{[12]}
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 estimated as 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 (1903 translation by Edwin Hamilton Gifford), or as 804,000,000 stadia (edition of Édouard des Places, dated 19741991). Using the Greek stadium of 185 to 190 metres,^{[13]}^{[14]} 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 2%).^{[15]} A similar measurement to that of Eratosthenes is reported in a Chinese mathematical treatise, the Zhoubi suanjing (1st century BCE), although contrary to Eratosthenes, it assumed that the Earth was flat.^{[16]}
Solar parallax 
Earth radii 


Ptolemy (2nd cent.)  2′ 50″  1,210 
Yaqūb ibn Tāriq (8th cent.)  25″  8,000 
Godefroy Wendelin (1635)  15″  14,000 
Jeremiah Horrocks (1639)  15″  14,000 
Christiaan Huygens (1659)  8.6″  24,000 
Cassini & Richer (1672)  9½″  21,700 
Jérôme Lalande (1771)  8.6″  24,000 
Simon Newcomb (1895)  8.80″  23,440 
Arthur Hinks (1909)  8.807″  23,420 
H. Spencer Jones (1941)  8.790″  23,466 
modern  8.794143″  23,455 
In the 2nd century CE, Ptolemy estimated the distance as 1,210 times the Earth radius,^{[17]} again about 20 times the distance to the Moon. This value was used by Islamic astronomers until the 11th century and by European astronomers until the 17th century. Abu Rayhan Biruni was the first to realize that the distance between the Earth and the Sun is much larger than Ptolemy's estimate in his Masudic Canon (1031), on the basis that Ptolemy had disregarded annular eclipses.^{[18]} In his India (1030), Biruni quoted an earlier 8thcentury estimate from Yaqūb ibn Tāriq's AzZīj alMahlul min asSindhind liDarajat Daraja, which listed the greatest distance between the Earth and the Sun as 8,000 times the Earth's radius.^{[19]} Later Islamic astronomers such as Jabir ibn Aflah in the 12th century and Mo'ayyeduddin Urdi in the 13th century also realized that Ptolemy grossly underestimated the distance to the Sun.^{[20]}
In Europe, Johannes Kepler was the first to realize that Ptolemy's estimate must be too low (according to Kepler, at least by a factor of three) in his Rudolphine Tables (1627). Kepler's laws of planetary motion allowed astronomers to calculate the relative distances of the planets from the Sun, and rekindled interest in measuring the absolute value for the Earth (which could then be applied to the other planets). The invention of the telescope allowed far more accurate measurements of angles than is possible with the naked eye. Flemish astronomer Godefroy Wendelin repeated Aristarchus' measurements in 1635, and found that Ptolemy's value was too low by a factor of at least eleven.
A somewhat more accurate estimate can be obtained by observing the transit of Venus. By measuring the transit in two different locations, one can accurately calculate the parallax of Venus and from the relative distance of the Earth and Venus from the Sun, the solar parallax α (which cannot be measured directly^{[21]}). Jeremiah Horrocks had attempted to produce an estimate based on his observation of the 1639 transit (published in 1662), giving a solar parallax of 15 arcseconds, similar to Wendelin's figure. The solar parallax is related to the Earth–Sun distance as measured in Earth radii by
The smaller the solar parallax, the greater the distance between the Sun and the Earth: a solar parallax of 15" is equivalent to an Earth–Sun distance of 13,750 Earth radii.
Christiaan Huygens believed the distance was even greater: by comparing the apparent sizes of Venus and Mars, he estimated a value of about 24,000 Earth radii,^{[22]} equivalent to a solar parallax of 8.6". Although Huygens estimate is remarkably close to modern values, it is often discounted by historians of astronomy because of the many unproven (and false) assumptions he had to make for his method to work: the accuracy of his value seems to based more on luck than good measurement, with his various errors cancelling each other out.
Jean Richer and Giovanni Domenico Cassini measured the parallax of Mars between Paris and Cayenne in French Guiana when Mars was at its closest to Earth in 1672. They arrived at a figure for the solar parallax of 9½", equivalent to an Earth–Sun distance of about 22,000 Earth radii. They were also the first astronomers to have access to an accurate and reliable value for the radius of the Earth, which had been measured by their colleague Jean Picard in 1669 as 3,269 thousand toises. Another colleague, Ole Rømer, discovered the finite speed of light in 1676: the speed was so great that it was usually quoted as the time required for light to travel from the Sun to the Earth, or "light time per unit distance", a convention that is still followed by astronomers today.
A better method for observing Venus transits was devised by James Gregory and published in his Optica Promata (1663). It was strongly advocated by Edmond Halley^{[23]} and was applied to the transits of Venus observed in 1761 and 1769, and then again in 1874 and 1882. Transits of Venus occur in pairs, but less than one pair every century, and the observations of the transits in 1761 and 1769 was an unprecedented international scientific operation. Despite the Seven Years' War, dozens of astronomers were dispatched to observing points around the world at great expense and personal danger: several of them died in the endeavour.^{[24]} The various results were collated by Jérôme Lalande to give a figure for the solar parallax of 8.6″.
Date  Method  A/Gm  Uncertainty 

1895  aberration  149.25  0.12 
1941  parallax  149.674  0.016 
1964  radar  149.5981  0.001 
1976  telemetry  149.597 870  0.000 001 
2009  telemetry  149.597 870 700  0.000 000 003 
Another method involved determining the constant of 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 8.794143″), although Newcomb also used data from the transits of Venus. Newcomb also collaborated with A. A. Michelson to measure the speed of light with Earthbased equipment: combined with the constant of aberration (which is related to the light time per unit distance) this gave the first direct measurement of the Earth–Sun distance in kilometres. Newcomb's value for the solar parallax (and for the constant of aberration and the Gaussian gravitational constant) were incorporated into the first international system of astronomical constants in 1896,^{[25]} which remained in place for the calculation of ephemerides until 1964.^{[26]} The name "astronomical unit" appears first to have been used in 1903.^{[27]}
The discovery of the nearEarth asteroid 433 Eros and its passage near the Earth in 1900–1901 allowed a considerable improvement in parallax measurement.^{[28]} Another international project to measure the parallax of 433 Eros was undertaken in 1930–1931.^{[21]}^{[29]}
Direct radar measurements of the distances to Venus and Mars became available in the early 1960s. Along with improved measurements of the speed of light, these showed that Newcomb's values for the solar parallax and the constant of aberration were inconsistent with one another.^{[30]}
The unit distance A (the value of the astronomical unit in metres) can be expressed in term of other astronomical constants:
where G is the Newtonian gravitational constant, M_{☉} is the solar mass, k is the Gaussian gravitational constant and D is the time period of one day. The sun is constantly losing mass by radiating away energy,^{[31]} so the orbits of the planets are steadily expanding outward from the sun. This has led to calls to abandon the astronomical unit as a unit of measurement.^{[32]} There have also been calls to redefine the astronomical unit in terms of a fixed number of metres.^{[33]}
As the speed of light has an exact defined value in SI units and the Gaussian gravitational constant k is fixed in the astronomical system of units, measuring the light time per unit distance is exactly equivalent to measuring the product GM_{☉} in SI units. Hence, it is possible to construct ephemerides entirely in SI units, which is increasing becoming the norm.
In 2004, an analysis of radiometric measurements in the inner Solar System suggested that the secular increase in the unit distance was much larger than can be accounted for by solar radiation, +15±4 metres per century.^{[34]} Later estimates based on both radiometric and angular observations lowered this estimate to +7±2 metres per century,^{[35]} but this is still far larger than can be accounted for by solar radiation and current theories of gravitation.^{[36]} The possible variation in the gravitational constant based on radiometric measurements is of the order of parts in 10^{12} per century, or lower.^{[37]} It has been suggested that the observed increase could be explained by the DGP model.^{[38]}
The distances are approximate mean distances. It has to be taken into consideration that the distances between celestial bodies change in time due to their orbits and other factors.

SI units  

149.60×10^{6} km  149.60×10^{9} m 
Astronomical units  
4.8481×10^{6} pc  15.813×10^{−6} ly}} 
US customary / Imperial units  
92.956×10^{6} mi  490.81×10^{9} ft 
The astronomical unit (AU or au or a.u. or sometimes ua) is a unit of length about the same as the mean distance from the center of the Earth to the center of the Sun. The currently accepted value of the AU is 149,597,870,691 meters (usually stated as 150 million kilometers or 93 million miles).
Astronomers usually measure distances within the Solar System in astronomical units. Mars is about 1.4 AU from the Sun, Jupiter lies at roughly 5.2 AU, and Neptune is roughly 30 AU from the Sun.
Astronomical unit is a term that is important to remember and consider when we try to understand the universe.
