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Uranus
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This article is about the planet. For other uses, see Uranus (disambiguation).
Uranus
Uranus as a featureless disc, photographed by Voyager 2 in 1986
Discovery
Discovered by
William Herschel
Discovery date
March 13, 1781
Designations
Pronunciation
/ˈjʊərənəs/ ( listen) or /jʊəˈreɪnəs/ ( listen)[1][2]
Adjectives
Uranian
Orbital characteristics[7][a]
Epoch J2000
Aphelion
7012300841317977700♠20.11 AU
(7012300800000000000♠3,008 Gm)
Perihelion
7012274212896993099♠18.33 AU
(7012274200000000000♠2,742 Gm)
Semi-major axis
7012287503171826088♠19.2184 AU
(7012287504000000000♠2,875.04 Gm)
Eccentricity
6998463810000000000♠0.046381
Orbital period
7001840205000000000♠84.0205 yr
7009265148640000000♠30,688.5 d[3]
7004427180000000000♠42,718 Uranian solar days[4]
Synodic period
369.66 days[5]
Average orbital speed
6.80 km/s[5]
Mean anomaly
7000248253189342721♠142.238600°
Inclination
6998134913951179161♠0.773° to ecliptic
6.48° to Sun's equator
1.02° to invariable plane[6]
Longitude of ascending node
7000129164836623092♠74.006°
Argument of perihelion
7000169294942532115♠96.998857°
Known satellites
27
Physical characteristics
Mean radius
7007253620000000000♠25,362±7 km[8][b]
Equatorial radius
7007255590000000000♠25,559±4 km
4.007 Earths[8][b]
Polar radius
7007249730000000000♠24,973±20 km
3.929 Earths[8][b]
Flattening
6998229000000000000♠0.0229±0.0008[c]
Circumference
7008159354100000000♠159,354.1 km[3]
Surface area
7015811560000000000♠8.1156×109 km2[3][b]
15.91 Earths
Volume
7022683300000000000♠6.833×1013 km3[5][b]
63.086 Earths
Mass
7025868100000000000♠(8.6810±0.0013)×1025 kg
14.536 Earths[9]
GM=7006579393900000000♠5,793,939±13 km3/s2
Mean density
7003127000000000000♠1.27 g/cm3[5][d]
Surface gravity
7000869000000000000♠8.69 m/s2[5][b]
0.886 g
Moment of inertia factor
6999230000000000000♠0.23[10] (estimate)
Escape velocity
21.3 km/s[5][b]
Sidereal rotation period
2995379362880000000♠−0.71833 d (retrograde)
17 h 14 min 24 s[8]
Equatorial rotation velocity
2.59 km/s
9,320 km/h
Axial tilt
97.77° (to orbit)[5]
North pole right ascension
17h 9m 15s
257.311°[8]
North pole declination
−15.175°[8]
Albedo
0.300 (Bond)
0.51 (geom.)[5]
Surface temp.
min
mean
max
1 bar level[11]
76 K (−197.2 °C)
0.1 bar
(tropopause)[12]
47 K 53 K 57 K
Apparent magnitude
5.9[13] to 5.32[5]
Angular diameter
3.3″ to 4.1″[5]
Atmosphere[12][14][15][e]
Scale height
27.7 km[5]
Composition by volume
(Below 1.3 bar)
Gases:
83 ± 3% hydrogen (H2)
15 ± 3% helium (He)
2.3% methane (CH4)
0.009% (0.007–0.015%) hydrogen deuteride (HD)
Ices:
ammonia (NH3)
water (H2O)
ammonium hydrosulfide (NH4SH)
methane hydrate
Uranus is the seventh planet from the Sun. It has the third-largest planetary radius and fourth-largest planetary mass in the Solar System. Uranus is similar in composition to Neptune, and both have different bulk chemical composition from that of the larger gas giants Jupiter and Saturn. For this reason, scientists often classify Uranus and Neptune as "ice giants" to distinguish them from the gas giants. Uranus's atmosphere is similar to Jupiter's and Saturn's in its primary composition of hydrogen and helium, but it contains more "ices" such as water, ammonia, and methane, along with traces of other hydrocarbons.[12] It is the coldest planetary atmosphere in the Solar System, with a minimum temperature of 49 K (−224 °C; −371 °F), and has a complex, layered cloud structure with water thought to make up the lowest clouds and methane the uppermost layer of clouds.[12] The interior of Uranus is mainly composed of ices and rock.[11]
Uranus is the only planet whose name is derived directly from a figure from Greek mythology, from the Latinised version of the Greek god of the sky Ouranos. Like the other giant planets, Uranus has a ring system, a magnetosphere, and numerous moons. The Uranian system has a unique configuration among those of the planets because its axis of rotation is tilted sideways, nearly into the plane of its solar orbit. Its north and south poles, therefore, lie where most other planets have their equators.[16] In 1986, images from Voyager 2 showed Uranus as an almost featureless planet in visible light, without the cloud bands or storms associated with the other giant planets.[16] Observations from Earth have shown seasonal change and increased weather activity as Uranus approached its equinox in 2007. Wind speeds can reach 250 metres per second (900 km/h; 560 mph).[17]
Contents
[hide]
1 History
1.1 Discovery
1.2 Name
2 Orbit and rotation
2.1 Axial tilt
2.2 Visibility
3 Physical characteristics
3.1 Internal structure
3.1.1 Internal heat
3.2 Atmosphere
3.2.1 Composition
3.2.2 Troposphere
3.2.3 Upper atmosphere
3.3 Magnetosphere
4 Climate
4.1 Banded structure, winds and clouds
4.2 Seasonal variation
5 Formation
6 Moons
6.1 Planetary rings
7 Exploration
8 In culture
9 See also
10 Notes
11 References
12 Further reading
13 External links
History
Like the classical planets, Uranus is visible to the naked eye, but it was never recognised as a planet by ancient observers because of its dimness and slow orbit.[18] Sir William Herschel announced its discovery on 13 March 1781, expanding the known boundaries of the Solar System for the first time in history and making Uranus the first planet discovered with a telescope.
Discovery
"34 Tauri" redirects here. For the Firefly Verse, see List of Firefly planets and moons.
William Herschel, discoverer of Uranus
Replica of the telescope used by Herschel to discover Uranus
Uranus had been observed on many occasions before its recognition as a planet, but it was generally mistaken for a star. Possibly the earliest known observation was by Hipparchos, who in 128 BC might have recorded it as a star for his star catalogue that was later incorporated into Ptolemy's Almagest.[19] The earliest definite sighting was in 1690, when John Flamsteed observed it at least six times, cataloguing it as 34 Tauri. The French astronomer Pierre Charles Le Monnier observed Uranus at least twelve times between 1750 and 1769,[20] including on four consecutive nights.
Sir William Herschel observed Uranus on 13 March 1781 from the garden of his house at 19 New King Street in Bath, Somerset, England (now the Herschel Museum of Astronomy),[21] and initially reported it (on 26 April 1781) as a comet.[22] Herschel "engaged in a series of observations on the parallax of the fixed stars",[23] using a telescope of his own design.
Herschel recorded in his journal: "In the quartile near ζ Tauri ... either [a] Nebulous star or perhaps a comet."[24] On 17 March he noted: "I looked for the Comet or Nebulous Star and found that it is a Comet, for it has changed its place."[25] When he presented his discovery to the Royal Society, he continued to assert that he had found a comet, but also implicitly compared it to a planet:[23]
The power I had on when I first saw the comet was 227. From experience I know that the diameters of the fixed stars are not proportionally magnified with higher powers, as planets are; therefore I now put the powers at 460 and 932, and found that the diameter of the comet increased in proportion to the power, as it ought to be, on the supposition of its not being a fixed star, while the diameters of the stars to which I compared it were not increased in the same ratio. Moreover, the comet being magnified much beyond what its light would admit of, appeared hazy and ill-defined with these great powers, while the stars preserved that lustre and distinctness which from many thousand observations I knew they would retain. The sequel has shown that my surmises were well-founded, this proving to be the Comet we have lately observed.[23]
Herschel notified the Astronomer Royal Nevil Maskelyne of his discovery and received this flummoxed reply from him on 23 April 1781: "I don't know what to call it. It is as likely to be a regular planet moving in an orbit nearly circular to the sun as a Comet moving in a very eccentric ellipsis. I have not yet seen any coma or tail to it."[26]
Although Herschel continued to describe his new object as a comet, other astronomers had already begun to suspect otherwise. Finnish-Swedish astronomer Anders Johan Lexell, working in Russia, was the first to compute the orbit of the new object.[27] Its nearly circular orbit led him to a conclusion that it was a planet rather than a comet. Berlin astronomer Johann Elert Bode described Herschel's discovery as "a moving star that can be deemed a hitherto unknown planet-like object circulating beyond the orbit of Saturn".[28] Bode concluded that its near-circular orbit was more like a planet than a comet.[29]
The object was soon universally accepted as a new planet. By 1783, Herschel acknowledged this to Royal Society president Joseph Banks: "By the observation of the most eminent Astronomers in Europe it appears that the new star, which I had the honour of pointing out to them in March 1781, is a Primary Planet of our Solar System."[30] In recognition of his achievement, King George III gave Herschel an annual stipend of £200 on condition that he move to Windsor so that the Royal Family could look through his telescopes.[31]
Name
The name of Uranus references the ancient Greek deity of the sky Uranus (Ancient Greek: Οὐρανός), the father of Cronus (Saturn) and grandfather of Zeus (Jupiter), which in Latin became "Ūranus" (Latin pronunciation: [ˈuːranʊs]).[1] It is the only planet whose name is derived directly from a figure of Greek mythology. The adjectival form of Uranus is "Uranian".[32] The pronunciation of the name Uranus preferred among astronomers is /ˈjʊərənəs/,[2] with stress on the first syllable as in Latin Ūranus, in contrast to /jʊəˈreɪnəs/, with stress on the second syllable and a long a, though both are considered acceptable.[f]
Consensus on the name was not reached until almost 70 years after the planet's discovery. During the original discussions following discovery, Maskelyne asked Herschel to "do the astronomical world the faver [sic] to give a name to your planet, which is entirely your own, [and] which we are so much obliged to you for the discovery of".[34] In response to Maskelyne's request, Herschel decided to name the object Georgium Sidus (George's Star), or the "Georgian Planet" in honour of his new patron, King George III.[35] He explained this decision in a letter to Joseph Banks:[30]
In the fabulous ages of ancient times the appellations of Mercury, Venus, Mars, Jupiter and Saturn were given to the Planets, as being the names of their principal heroes and divinities. In the present more philosophical era it would hardly be allowable to have recourse to the same method and call it Juno, Pallas, Apollo or Minerva, for a name to our new heavenly body. The first consideration of any particular event, or remarkable incident, seems to be its chronology: if in any future age it should be asked, when this last-found Planet was discovered? It would be a very satisfactory answer to say, 'In the reign of King George the Third'.
Herschel's proposed name was not popular outside Britain, and alternatives were soon proposed. Astronomer Jérôme Lalande proposed that it be named Herschel in honour of its discoverer.[36] Swedish astronomer Erik Prosperin proposed the name Neptune, which was supported by other astronomers who liked the idea to commemorate the victories of the British Royal Naval fleet in the course of the American Revolutionary War by calling the new planet even Neptune George III or Neptune Great Britain.[27]
In a March 1782 treatise, Bode proposed Uranus, the Latinised version of the Greek god of the sky, Ouranos.[37] Bode argued that the name should follow the mythology so as not to stand out as different from the other planets, and that Uranus was an appropriate name as the father of the first generation of the Titans.[37] He also noted that elegance of the name in that just as Saturn was the father of Jupiter, the new planet should be named after the father of Saturn.[31][37][38][39] In 1789, Bode's Royal Academy colleague Martin Klaproth named his newly discovered element uranium in support of Bode's choice.[40] Ultimately, Bode's suggestion became the most widely used, and became universal in 1850 when HM Nautical Almanac Office, the final holdout, switched from using Georgium Sidus to Uranus.[38]
Uranus has two astronomical symbols. The first to be proposed, ♅,[g] was suggested by Lalande in 1784. In a letter to Herschel, Lalande described it as "un globe surmonté par la première lettre de votre nom" ("a globe surmounted by the first letter of your surname").[36] A later proposal, ⛢,[h] is a hybrid of the symbols for Mars and the Sun because Uranus was the Sky in Greek mythology, which was thought to be dominated by the combined powers of the Sun and Mars.[41]
Uranus is called by a variety of translations in other languages. In Chinese, Japanese, Korean, and Vietnamese, its name is literally translated as the "sky king star" (天王星).[42][43][44][45] In Thai, its official name is Dao Yurenat (ดาวยูเรนัส), as in English. Its other name in Thai is Dao Maritayu (ดาวมฤตยู, Star of Mṛtyu), after the Sanskrit word for "death", Mrtyu (मृत्यु). In Mongolian, its name is Tengeriin Van (Тэнгэрийн ван), translated as "King of the Sky", reflecting its namesake god's role as the ruler of the heavens. In Hawaiian, its name is Hele‘ekala. In Māori, its name is Whērangi.[46][47]
Orbit and rotation
A 1998 false-colour near-infrared image of Uranus showing cloud bands, rings, and moons obtained by the Hubble Space Telescope's NICMOS camera.
Uranus orbits the Sun once every 84 years. Its average distance from the Sun is roughly 20 AU (3 billion km; 2 billion mi). The difference between its minimum and maximum distance from the Sun is 1.8 AU, larger than that of any other planet, though not as large as that of pluto, the nearest dwarf planet.[48] The intensity of sunlight varies inversely with the square of distance, and so on Uranus (at about 20 times the distance from the Sun compared to Earth) it is about 1/400 the intensity of light on Earth.[49] Its orbital elements were first calculated in 1783 by Pierre-Simon Laplace.[50] With time, discrepancies began to appear between the predicted and observed orbits, and in 1841, John Couch Adams first proposed that the differences might be due to the gravitational tug of an unseen planet. In 1845, Urbain Le Verrier began his own independent research into Uranus's orbit. On 23 September 1846, Johann Gottfried Galle located a new planet, later named Neptune, at nearly the position predicted by Le Verrier.[51]
The rotational period of the interior of Uranus is 17 hours, 14 minutes. As on all the giant planets, its upper atmosphere experiences strong winds in the direction of rotation. At some latitudes, such as about 60 degrees south, visible features of the atmosphere move much faster, making a full rotation in as little as 14 hours.[52]
Axial tilt
The Uranian axis of rotation is approximately parallel with the plane of the Solar System, with an axial tilt of 97.77° (as defined by prograde rotation). This gives it seasonal changes completely unlike those of the other planets. Near the solstice, one pole faces the Sun continuously and the other faces away. Only a narrow strip around the equator experiences a rapid day–night cycle, but with the Sun low over the horizon. At the other side of Uranus's orbit the orientation of the poles towards the Sun is reversed. Each pole gets around 42 years of continuous sunlight, followed by 42 years of darkness.[53] Near the time of the equinoxes, the Sun faces the equator of Uranus giving a period of day–night cycles similar to those seen on most of the other planets.
Uranus reached its most recent equinox on 7 December 2007.[54][55]
Northern hemisphere
Year
Southern hemisphere
Winter solstice 1902, 1986 Summer solstice
Vernal equinox 1923, 2007 Autumnal equinox
Summer solstice 1944, 2028 Winter solstice
Autumnal equinox 1965, 2049 Vernal equinox
One result of this axis orientation is that, averaged over the Uranian year, the polar regions of Uranus receive a greater energy input from the Sun than its equatorial regions. Nevertheless, Uranus is hotter at its equator than at its poles. The underlying mechanism that causes this is unknown. The reason for Uranus's unusual axial tilt is also not known with certainty, but the usual speculation is that during the formation of the Solar System, an Earth-sized protoplanet collided with Uranus, causing the skewed orientation.[56] Uranus's south pole was pointed almost directly at the Sun at the time of Voyager 2's flyby in 1986. The labelling of this pole as "south" uses the definition currently endorsed by the International Astronomical Union, namely that the north pole of a planet or satellite is the pole that points above the invariable plane of the Solar System, regardless of the direction the planet is spinning.[57][58] A different convention is sometimes used, in which a body's north and south poles are defined according to the right-hand rule in relation to the direction of rotation.[59]
Visibility
From 1995 to 2006, Uranus's apparent magnitude fluctuated between +5.6 and +5.9, placing it just within the limit of naked eye visibility at +6.5.[13] Its angular diameter is between 3.4 and 3.7 arcseconds, compared with 16 to 20 arcseconds for Saturn and 32 to 45 arcseconds for Jupiter.[13] At opposition, Uranus is visible to the naked eye in dark skies, and becomes an easy target even in urban conditions with binoculars.[5] In larger amateur telescopes with an objective diameter of between 15 and 23 cm, Uranus appears as a pale cyan disk with distinct limb darkening. With a large telescope of 25 cm or wider, cloud patterns, as well as some of the larger satellites, such as Titania and Oberon, may be visible.[60]
Physical characteristics
Internal structure
Size comparison of Earth and Uranus
Diagram of the interior of Uranus
Uranus's mass is roughly 14.5 times that of Earth, making it the least massive of the giant planets. Its diameter is slightly larger than Neptune's at roughly four times that of Earth. A resulting density of 1.27 g/cm3 makes Uranus the second least dense planet, after Saturn.[8][9] This value indicates that it is made primarily of various ices, such as water, ammonia, and methane.[11] The total mass of ice in Uranus's interior is not precisely known, because different figures emerge depending on the model chosen; it must be between 9.3 and 13.5 Earth masses.[11][61] Hydrogen and helium constitute only a small part of the total, with between 0.5 and 1.5 Earth masses.[11] The remainder of the non-ice mass (0.5 to 3.7 Earth masses) is accounted for by rocky material.[11]
The standard model of Uranus's structure is that it consists of three layers: a rocky (silicate/iron–nickel) core in the centre, an icy mantle in the middle and an outer gaseous hydrogen/helium envelope.[11][62] The core is relatively small, with a mass of only 0.55 Earth masses and a radius less than 20% of Uranus's; the mantle comprises its bulk, with around 13.4 Earth masses, and the upper atmosphere is relatively insubstantial, weighing about 0.5 Earth masses and extending for the last 20% of Uranus's radius.[11][62] Uranus's core density is around 9 g/cm3, with a pressure in the centre of 8 million bars (800 GPa) and a temperature of about 5000 K.[61][62] The ice mantle is not in fact composed of ice in the conventional sense, but of a hot and dense fluid consisting of water, ammonia and other volatiles.[11][62] This fluid, which has a high electrical conductivity, is sometimes called a water–ammonia ocean.[63]
The extreme pressure and temperature deep within Uranus may break up the methane molecules, with the carbon atoms condensing into crystals of diamond that rain down through the mantle like hailstones.[64][65][66] Very-high-pressure experiments at the Lawrence Livermore National Laboratory suggest that the base of the mantle may comprise an ocean of liquid diamond, with floating solid 'diamond-bergs'.[67][68]
The bulk compositions of Uranus and Neptune are different from those of Jupiter and Saturn, with ice dominating over gases, hence justifying their separate classification as ice giants. There may be a layer of ionic water where the water molecules break down into a soup of hydrogen and oxygen ions, and deeper down superionic water in which the oxygen crystallises but the hydrogen ions move freely within the oxygen lattice.[69]
Although the model considered above is reasonably standard, it is not unique; other models also satisfy observations. For instance, if substantial amounts of hydrogen and rocky material are mixed in the ice mantle, the total mass of ices in the interior will be lower, and, correspondingly, the total mass of rocks and hydrogen will be higher. Presently available data does not allow a scientific determination which model is correct.[61] The fluid interior structure of Uranus means that it has no solid surface. The gaseous atmosphere gradually transitions into the internal liquid layers.[11] For the sake of convenience, a revolving oblate spheroid set at the point at which atmospheric pressure equals 1 bar (100 kPa) is conditionally designated as a "surface". It has equatorial and polar radii of 25,559 ± 4 km (15,881.6 ± 2.5 mi) and 24,973 ± 20 km (15,518 ± 12 mi), respectively.[8] This surface is used throughout this article as a zero point for altitudes.
Internal heat
Uranus's internal heat appears markedly lower than that of the other giant planets; in astronomical terms, it has a low thermal flux.[17][70] Why Uranus's internal temperature is so low is still not understood. Neptune, which is Uranus's near twin in size and composition, radiates 2.61 times as much energy into space as it receives from the Sun,[17] but Uranus radiates hardly any excess heat at all. The total power radiated by Uranus in the far infrared (i.e. heat) part of the spectrum is 7000106000000000000♠1.06±0.08 times the solar energy absorbed in its atmosphere.[12][71] Uranus's heat flux is only 6998420000000000000♠0.042±0.047 W/m2, which is lower than the internal heat flux of Earth of about 6998750000000000000♠0.075 W/m2.[71] The lowest temperature recorded in Uranus's tropopause is 49 K (−224.2 °C; −371.5 °F), making Uranus the coldest planet in the Solar System.[12][71]
One of the hypotheses for this discrepancy suggests that when Uranus was hit by a supermassive impactor, which caused it to expel most of its primordial heat, it was left with a depleted core temperature.[72] This impact hypothesis is also used in some attempts to explain the planet's axial tilt. Another hypothesis is that some form of barrier exists in Uranus's upper layers that prevents the core's heat from reaching the surface.[11] For example, convection may take place in a set of compositionally different layers, which may inhibit the upward heat transport;[12][71] perhaps double diffusive convection is a limiting factor.[11]
Atmosphere
Main article: Atmosphere of Uranus
Although there is no well-defined solid surface within Uranus's interior, the outermost part of Uranus's gaseous envelope that is accessible to remote sensing is called its atmosphere.[12] Remote-sensing capability extends down to roughly 300 km below the 1 bar (100 kPa) level, with a corresponding pressure around 100 bar (10 MPa) and temperature of 320 K (47 °C; 116 °F).[73] The tenuous thermosphere extends over two planetary radii from the nominal surface, which is defined to lie at a pressure of 1 bar.[74] The Uranian atmosphere can be divided into three layers: the troposphere, between altitudes of −300 and 50 km (−186 and 31 mi) and pressures from 100 to 0.1 bar (10 MPa to 10 kPa); the stratosphere, spanning altitudes between 50 and 4,000 km (31 and 2,485 mi) and pressures of between 0.1 and 10−10 bar (10 kPa to 10 µPa); and the thermosphere extending from 4,000 km to as high as 50,000 km from the surface.[12] There is no mesosphere.
Composition
The composition of Uranus's atmosphere is different from its bulk, consisting mainly of molecular hydrogen and helium.[12] The helium molar fraction, i.e. the number of helium atoms per molecule of gas, is 6999150000000000000♠0.15±0.03[15] in the upper troposphere, which corresponds to a mass fraction 6999260000000000000♠0.26±0.05.[12][71] This value is close to the protosolar helium mass fraction of 6999275000000000000♠0.275±0.01,[75] indicating that helium has not settled in its centre as it has in the gas giants.[12] The third-most-abundant component of Uranus's atmosphere is methane (CH
4).[12] Methane has prominent absorption bands in the visible and near-infrared (IR), making Uranus aquamarine or cyan in colour.[12] Methane molecules account for 2.3% of the atmosphere by molar fraction below the methane cloud deck at the pressure level of 1.3 bar (130 kPa); this represents about 20 to 30 times the carbon abundance found in the Sun.[12][14][76] The mixing ratio[i] is much lower in the upper atmosphere due to its extremely low temperature, which lowers the saturation level and causes excess methane to freeze out.[77] The abundances of less volatile compounds such as ammonia, water, and hydrogen sulfide in the deep atmosphere are poorly known. They are probably also higher than solar values.[12][78] Along with methane, trace amounts of various hydrocarbons are found in the stratosphere of Uranus, which are thought to be produced from methane by photolysis induced by the solar ultraviolet (UV) radiation.[79] They include ethane (C
2H
6), acetylene (C
2H
2), methylacetylene (CH
3C
2H), and diacetylene (C
2HC
2H).[77][80][81] Spectroscopy has also uncovered traces of water vapour, carbon monoxide and carbon dioxide in the upper atmosphere, which can only originate from an external source such as infalling dust and comets.[80][81][82]
Troposphere
The troposphere is the lowest and densest part of the atmosphere and is characterised by a decrease in temperature with altitude.[12] The temperature falls from about 320 K (47 °C; 116 °F) at the base of the nominal troposphere at −300 km to 53 K (−220 °C; −364 °F) at 50 km.[73][76] The temperatures in the coldest upper region of the troposphere (the tropopause) actually vary in the range between 49 and 57 K (−224 and −216 °C; −371 and −357 °F) depending on planetary latitude.[12][70] The tropopause region is responsible for the vast majority of Uranus's thermal far infrared emissions, thus determining its effective temperature of 59.1 ± 0.3 K (−214.1 ± 0.3 °C; −353.3 ± 0.5 °F).[70][71]
The troposphere is thought to have a highly complex cloud structure; water clouds are hypothesised to lie in the pressure range of 50 to 100 bar (5 to 10 MPa), ammonium hydrosulfide clouds in the range of 20 to 40 bar (2 to 4 MPa), ammonia or hydrogen sulfide clouds at between 3 and 10 bar (0.3 and 1 MPa) and finally directly detected thin methane clouds at 1 to 2 bar (0.1 to 0.2 MPa).[12][14][73][83] The troposphere is a dynamic part of the atmosphere, exhibiting strong winds, bright clouds and seasonal changes.[17]
Upper atmosphere
Aurorae on Uranus taken by the Space Telescope Imaging Spectrograph (STIS) installed on Hubble.[84]
The middle layer of the Uranian atmosphere is the stratosphere, where temperature generally increases with altitude from 53 K (−220 °C; −364 °F) in the tropopause to between 800 and 850 K (527 and 577 °C; 980 and 1,070 °F) at the base of the thermosphere.[74] The heating of the stratosphere is caused by absorption of solar UV and IR radiation by methane and other hydrocarbons,[85] which form in this part of the atmosphere as a result of methane photolysis.[79] Heat is also conducted from the hot thermosphere.[85] The hydrocarbons occupy a relatively narrow layer at altitudes of between 100 and 300 km corresponding to a pressure range of 10 to 0.1 mbar (10.00 to 0.10 hPa) and temperatures of between 75 and 170 K (−198 and −103 °C; −325 and −154 °F).[77][80] The most abundant hydrocarbons are methane, acetylene and ethane with mixing ratios of around 10−7 relative to hydrogen. The mixing ratio of carbon monoxide is similar at these altitudes.[77][80][82] Heavier hydrocarbons and carbon dioxide have mixing ratios three orders of magnitude lower.[80] The abundance ratio of water is around 7×10−9.[81] Ethane and acetylene tend to condense in the colder lower part of stratosphere and tropopause (below 10 mBar level) forming haze layers,[79] which may be partly responsible for the bland appearance of Uranus. The concentration of hydrocarbons in the Uranian stratosphere above the haze is significantly lower than in the stratospheres of the other giant planets.[77][86]
The outermost layer of the Uranian atmosphere is the thermosphere and corona, which has a uniform temperature around 800 to 850 K.[12][86] The heat sources necessary to sustain such a high level are not understood, as neither the solar UV nor the auroral activity can provide the necessary energy to maintain these temperatures. The weak cooling efficiency due to the lack of hydrocarbons in the stratosphere above 0.1 mBar pressure level may contribute too.[74][86] In addition to molecular hydrogen, the thermosphere-corona contains many free hydrogen atoms. Their small mass and high temperatures explain why the corona extends as far as 50,000 km (31,000 mi), or two Uranian radii, from its surface.[74][86] This extended corona is a unique feature of Uranus.[86] Its effects include a drag on small particles orbiting Uranus, causing a general depletion of dust in the Uranian rings.[74] The Uranian thermosphere, together with the upper part of the stratosphere, corresponds to the ionosphere of Uranus.[76] Observations show that the ionosphere occupies altitudes from 2,000 to 10,000 km (1,200 to 6,200 mi).[76] The Uranian ionosphere is denser than that of either Saturn or Neptune, which may arise from the low concentration of hydrocarbons in the stratosphere.[86][87] The ionosphere is mainly sustained by solar UV radiation and its density depends on the solar activity.[88] Auroral activity is insignificant as compared to Jupiter and Saturn.[86][89]
Uranus's atmosphere
Temperature profile of the Uranian troposphere and lower stratosphere. Cloud and haze layers are also indicated.
Zonal wind speeds on Uranus. Shaded areas show the southern collar and its future northern counterpart. The red curve is a symmetrical fit to the data.
Magnetosphere
The magnetic field of Uranus as observed by Voyager 2 in 1986. S and N are magnetic south and north poles.
Before the arrival of Voyager 2, no measurements of the Uranian magnetosphere had been taken, so its nature remained a mystery. Before 1986, scientists had expected the magnetic field of Uranus to be in line with the solar wind, because it would then align with Uranus's poles that lie in the ecliptic.[90]
Voyager's observations revealed that Uranus's magnetic field is peculiar, both because it does not originate from its geometric centre, and because it is tilted at 59° from the axis of rotation.[90][91] In fact the magnetic dipole is shifted from the Uranus's centre towards the south rotational pole by as much as one third of the planetary radius.[90] This unusual geometry results in a highly asymmetric magnetosphere, where the magnetic field strength on the surface in the southern hemisphere can be as low as 0.1 gauss (10 µT), whereas in the northern hemisphere it can be as high as 1.1 gauss (110 µT).[90] The average field at the surface is 0.23 gauss (23 µT).[90] Studies of Voyager 2 data in 2017 suggest that this asymmetry causes Uranus's magnetosphere to connect with the solar wind once a Uranian day, opening the planet to the Sun's particles.[92] In comparison, the magnetic field of Earth is roughly as strong at either pole, and its "magnetic equator" is roughly parallel with its geographical equator.[91] The dipole moment of Uranus is 50 times that of Earth.[90][91] Neptune has a similarly displaced and tilted magnetic field, suggesting that this may be a common feature of ice giants.[91] One hypothesis is that, unlike the magnetic fields of the terrestrial and gas giants, which are generated within their cores, the ice giants' magnetic fields are generated by motion at relatively shallow depths, for instance, in the water–ammonia ocean.[63][93] Another possible explanation for the magnetosphere's alignment is that there are oceans of liquid diamond in Uranus's interior that would deter the magnetic field.[67]
Despite its curious alignment, in other respects the Uranian magnetosphere is like those of other planets: it has a bow shock at about 23 Uranian radii ahead of it, a magnetopause at 18 Uranian radii, a fully developed magnetotail, and radiation belts.[90][91][94] Overall, the structure of Uranus's magnetosphere is different from Jupiter's and more similar to Saturn's.[90][91] Uranus's magnetotail trails behind it into space for millions of kilometres and is twisted by its sideways rotation into a long corkscrew.[90][95]
Uranus's magnetosphere contains charged particles: mainly protons and electrons, with a small amount of H2+ ions.[91][94] No heavier ions have been detected. Many of these particles probably derive from the thermosphere.[94] The ion and electron energies can be as high as 4 and 1.2 megaelectronvolts, respectively.[94] The density of low-energy (below 1 kiloelectronvolt) ions in the inner magnetosphere is about 2 cm−3.[96] The particle population is strongly affected by the Uranian moons, which sweep through the magnetosphere, leaving noticeable gaps.[94] The particle flux is high enough to cause darkening or space weathering of their surfaces on an astronomically rapid timescale of 100,000 years.[94] This may be the cause of the uniformly dark colouration of the Uranian satellites and rings.[97] Uranus has relatively well developed aurorae, which are seen as bright arcs around both magnetic poles.[86] Unlike Jupiter's, Uranus's aurorae seem to be insignificant for the energy balance of the planetary thermosphere.[89]
Climate
Main article: Climate of Uranus
Uranus's southern hemisphere in approximate natural colour (left) and in shorter wavelengths (right), showing its faint cloud bands and atmospheric "hood" as seen by Voyager 2
At ultraviolet and visible wavelengths, Uranus's atmosphere is bland in comparison to the other giant planets, even to Neptune, which it otherwise closely resembles.[17] When Voyager 2 flew by Uranus in 1986, it observed a total of ten cloud features across the entire planet.[16][98] One proposed explanation for this dearth of features is that Uranus's internal heat appears markedly lower than that of the other giant planets. The lowest temperature recorded in Uranus's tropopause is 49 K (−224 °C; −371 °F), making Uranus the coldest planet in the Solar System.[12][71]
Banded structure, winds and clouds
In 1986, Voyager 2 found that the visible southern hemisphere of Uranus can be subdivided into two regions: a bright polar cap and dark equatorial bands.[16] Their boundary is located at about −45° of latitude. A narrow band straddling the latitudinal range from −45 to −50° is the brightest large feature on its visible surface.[16][99] It is called a southern "collar". The cap and collar are thought to be a dense region of methane clouds located within the pressure range of 1.3 to 2 bar (see above).[100] Besides the large-scale banded structure, Voyager 2 observed ten small bright clouds, most lying several degrees to the north from the collar.[16] In all other respects Uranus looked like a dynamically dead planet in 1986. Voyager 2 arrived during the height of Uranus's southern summer and could not observe the northern hemisphere. At the beginning of the 21st century, when the northern polar region came into view, the Hubble Space Telescope (HST) and Keck telescope initially observed neither a collar nor a polar cap in the northern hemisphere.[99] So Uranus appeared to be asymmetric: bright near the south pole and uniformly dark in the region north of the southern collar.[99] In 2007, when Uranus passed its equinox, the southern collar almost disappeared, and a faint northern collar emerged near 45° of latitude.[101]
The first dark spot observed on Uranus. Image obtained by the HST ACS in 2006.
In the 1990s, the number of the observed bright cloud features grew considerably partly because new high-resolution imaging techniques became available.[17] Most were found in the northern hemisphere as it started to become visible.[17] An early explanation—that bright clouds are easier to identify in its dark part, whereas in the southern hemisphere the bright collar masks them – was shown to be incorrect.[102][103] Nevertheless there are differences between the clouds of each hemisphere. The northern clouds are smaller, sharper and brighter.[103] They appear to lie at a higher altitude.[103] The lifetime of clouds spans several orders of magnitude. Some small clouds live for hours; at least one southern cloud may have persisted since the Voyager 2 flyby.[17][98] Recent observation also discovered that cloud features on Uranus have a lot in common with those on Neptune.[17] For example, the dark spots common on Neptune had never been observed on Uranus before 2006, when the first such feature dubbed Uranus Dark Spot was imaged.[104] The speculation is that Uranus is becoming more Neptune-like during its equinoctial season.[105]
The tracking of numerous cloud features allowed determination of zonal winds blowing in the upper troposphere of Uranus.[17] At the equator winds are retrograde, which means that they blow in the reverse direction to the planetary rotation. Their speeds are from −360 to −180 km/h (−220 to −110 mph).[17][99] Wind speeds increase with the distance from the equator, reaching zero values near ±20° latitude, where the troposphere's temperature minimum is located.[17][70] Closer to the poles, the winds shift to a prograde direction, flowing with Uranus's rotation. Wind speeds continue to increase reaching maxima at ±60° latitude before falling to zero at the poles.[17] Wind speeds at −40° latitude range from 540 to 720 km/h (340 to 450 mph). Because the collar obscures all clouds below that parallel, speeds between it and the southern pole are impossible to measure.[17] In contrast, in the northern hemisphere maximum speeds as high as 860 km/h (540 mph) are observed near +50° latitude.[17][99][106]
Seasonal variation
Uranus in 2005. Rings, southern collar and a bright cloud in the northern hemisphere are visible (HST ACS image).
For a short period from March to May 2004, large clouds appeared in the Uranian atmosphere, giving it a Neptune-like appearance.[103][107] Observations included record-breaking wind speeds of 820 km/h (510 mph) and a persistent thunderstorm referred to as "Fourth of July fireworks".[98] On 23 August 2006, researchers at the Space Science Institute (Boulder, Colorado) and the University of Wisconsin observed a dark spot on Uranus's surface, giving scientists more insight into Uranus's atmospheric activity.[104] Why this sudden upsurge in activity occurred is not fully known, but it appears that Uranus's extreme axial tilt results in extreme seasonal variations in its weather.[55][105] Determining the nature of this seasonal variation is difficult because good data on Uranus's atmosphere have existed for less than 84 years, or one full Uranian year. Photometry over the course of half a Uranian year (beginning in the 1950s) has shown regular variation in the brightness in two spectral bands, with maxima occurring at the solstices and minima occurring at the equinoxes.[108] A similar periodic variation, with maxima at the solstices, has been noted in microwave measurements of the deep troposphere begun in the 1960s.[109] Stratospheric temperature measurements beginning in the 1970s also showed maximum values near the 1986 solstice.[85] The majority of this variability is thought to occur owing to changes in the viewing geometry.[102]
There are some indications that physical seasonal changes are happening in Uranus. Although Uranus is known to have a bright south polar region, the north pole is fairly dim, which is incompatible with the model of the seasonal change outlined above.[105] During its previous northern solstice in 1944, Uranus displayed elevated levels of brightness, which suggests that the north pole was not always so dim.[108] This information implies that the visible pole brightens some time before the solstice and darkens after the equinox.[105] Detailed analysis of the visible and microwave data revealed that the periodical changes of brightness are not completely symmetrical around the solstices, which also indicates a change in the meridional albedo patterns.[105] In the 1990s, as Uranus moved away from its solstice, Hubble and ground-based telescopes revealed that the south polar cap darkened noticeably (except the southern collar, which remained bright),[100] whereas the northern hemisphere demonstrated increasing activity,[98] such as cloud formations and stronger winds, bolstering expectations that it should brighten soon.[103] This indeed happened in 2007 when it passed an equinox: a faint northern polar collar arose, and the southern collar became nearly invisible, although the zonal wind profile remained slightly asymmetric, with northern winds being somewhat slower than southern.[101]
The mechanism of these physical changes is still not clear.[105] Near the summer and winter solstices, Uranus's hemispheres lie alternately either in full glare of the Sun's rays or facing deep space. The brightening of the sunlit hemisphere is thought to result from the local thickening of the methane clouds and haze layers located in the troposphere.[100] The bright collar at −45° latitude is also connected with methane clouds.[100] Other changes in the southern polar region can be explained by changes in the lower cloud layers.[100] The variation of the microwave emission from Uranus is probably caused by changes in the deep tropospheric circulation, because thick polar clouds and haze may inhibit convection.[110] Now that the spring and autumn equinoxes are arriving on Uranus, the dynamics are changing and convection can occur again.[98][110]
Formation
Main article: Formation and evolution of the Solar System
For details of the evolution of Uranus's orbit, see Nice model.
Many argue that the differences between the ice giants and the gas giants extend to their formation.[111][112] The Solar System is hypothesised to have formed from a giant rotating ball of gas and dust known as the presolar nebula. Much of the nebula's gas, primarily hydrogen and helium, formed the Sun, and the dust grains collected together to form the first protoplanets. As the planets grew, some of them eventually accreted enough matter for their gravity to hold on to the nebula's leftover gas.[111][112] The more gas they held onto, the larger they became; the larger they became, the more gas they held onto until a critical point was reached, and their size began to increase exponentially. The ice giants, with only a few Earth masses of nebular gas, never reached that critical point.[111][112][113] Recent simulations of planetary migration have suggested that both ice giants formed closer to the Sun than their present positions, and moved outwards after formation (the Nice model).[111]
Moons
Main article: Moons of Uranus
See also: Timeline of discovery of Solar System planets and their natural satellites
Major moons of Uranus in order of increasing distance (left to right), at their proper relative sizes and albedos (collage of Voyager 2 photographs)
The Uranus System (NACO/VLT image)
Uranus has 27 known natural satellites.[113] The names of these satellites are chosen from characters in the works of Shakespeare and Alexander Pope.[62][114] The five main satellites are Miranda, Ariel, Umbriel, Titania, and Oberon.[62] The Uranian satellite system is the least massive among those of the giant planets; the combined mass of the five major satellites would be less than half that of Triton (largest moon of Neptune) alone.[9] The largest of Uranus's satellites, Titania, has a radius of only 788.9 km (490.2 mi), or less than half that of the Moon, but slightly more than Rhea, the second-largest satellite of Saturn, making Titania the eighth-largest moon in the Solar System. Uranus's satellites have relatively low albedos; ranging from 0.20 for Umbriel to 0.35 for Ariel (in green light).[16] They are ice–rock conglomerates composed of roughly 50% ice and 50% rock. The ice may include ammonia and carbon dioxide.[97][115]
Among the Uranian satellites, Ariel appears to have the youngest surface with the fewest impact craters and Umbriel's the oldest.[16][97] Miranda has fault canyons 20 km (12 mi) deep, terraced layers, and a chaotic variation in surface ages and features.[16] Miranda's past geologic activity is thought to have been driven by tidal heating at a time when its orbit was more eccentric than currently, probably as a result of a former 3:1 orbital resonance with Umbriel.[116] Extensional processes associated with upwelling diapirs are the likely origin of Miranda's 'racetrack'-like coronae.[117][118] Ariel is thought to have once been held in a 4:1 resonance with Titania.[119]
Uranus has at least one horseshoe orbiter occupying the Sun–Uranus L3 Lagrangian point—a gravitationally unstable region at 180° in its orbit, 83982 Crantor.[120][121] Crantor moves inside Uranus's co-orbital region on a complex, temporary horseshoe orbit. 2010 EU65 is also a promising Uranus horseshoe librator candidate.[121]
Planetary rings
Main article: Rings of Uranus
The Uranian rings are composed of extremely dark particles, which vary in size from micrometres to a fraction of a metre.[16] Thirteen distinct rings are presently known, the brightest being the ε ring. All except two rings of Uranus are extremely narrow – they are usually a few kilometres wide. The rings are probably quite young; the dynamics considerations indicate that they did not form with Uranus. The matter in the rings may once have been part of a moon (or moons) that was shattered by high-speed impacts. From numerous pieces of debris that formed as a result of those impacts, only a few particles survived, in stable zones corresponding to the locations of the present rings.[97][122]
William Herschel described a possible ring around Uranus in 1789. This sighting is generally considered doubtful, because the rings are quite faint, and in the two following centuries none were noted by other observers. Still, Herschel made an accurate description of the epsilon ring's size, its angle relative to Earth, its red colour, and its apparent changes as Uranus travelled around the Sun.[123][124] The ring system was definitively discovered on 10 March 1977 by James L. Elliot, Edward W. Dunham, and Jessica Mink using the Kuiper Airborne Observatory. The discovery was serendipitous; they planned to use the occultation of the star SAO 158687 (also known as HD 128598) by Uranus to study its atmosphere. When their observations were analysed, they found that the star had disappeared briefly from view five times both before and after it disappeared behind Uranus. They concluded that there must be a ring system around Uranus.[125] Later they detected four additional rings.[125] The rings were directly imaged when Voyager 2 passed Uranus in 1986.[16] Voyager 2 also discovered two additional faint rings, bringing the total number to eleven.[16]
In December 2005, the Hubble Space Telescope detected a pair of previously unknown rings. The largest is located twice as far from Uranus as the previously known rings. These new rings are so far from Uranus that they are called the "outer" ring system. Hubble also spotted two small satellites, one of which, Mab, shares its orbit with the outermost newly discovered ring. The new rings bring the total number of Uranian rings to 13.[126] In April 2006, images of the new rings from the Keck Observatory yielded the colours of the outer rings: the outermost is blue and the other one red.[127][128] One hypothesis concerning the outer ring's blue colour is that it is composed of minute particles of water ice from the surface of Mab that are small enough to scatter blue light.[127][129] In contrast, Uranus's inner rings appear grey.[127]
Uranus's rings
Animation about the discovering occultation in 1977. (Click on it to start)
Uranus has a complicated planetary ring system, which was the second such system to be discovered in the Solar System after Saturn's.[122]
Uranus's aurorae against its equatorial rings, imaged by the Hubble telescope. Unlike the aurorae of Earth and Jupiter, those of Uranus are not in line with its poles, due to its lopsided magnetic field.
Exploration
Main article: Exploration of Uranus
Crescent Uranus as imaged by Voyager 2 while en route to Neptune
In 1986, NASA's Voyager 2 interplanetary probe encountered Uranus. This flyby remains the only investigation of Uranus carried out from a short distance and no other visits are planned. Launched in 1977, Voyager 2 made its closest approach to Uranus on 24 January 1986, coming within 81,500 km (50,600 mi) of the cloudtops, before continuing its journey to Neptune. The spacecraft studied the structure and chemical composition of Uranus's atmosphere,[76] including its unique weather, caused by its axial tilt of 97.77°. It made the first detailed investigations of its five largest moons and discovered 10 new ones. It examined all nine of the system's known rings and discovered two more.[16][97][130] It also studied the magnetic field, its irregular structure, its tilt and its unique corkscrew magnetotail caused by Uranus's sideways orientation.[90]
Voyager 1 was unable to visit Uranus because investigation of Saturn's moon Titan was considered a priority. This trajectory took Voyager 1 out of the plane of the ecliptic, ending its planetary science mission.[131]:118
The possibility of sending the Cassini spacecraft from Saturn to Uranus was evaluated during a mission extension planning phase in 2009, but was ultimately rejected in favour of destroying it in the Saturnian atmosphere.[132] It would have taken about twenty years to get to the Uranian system after departing Saturn.[132] A Uranus orbiter and probe was recommended by the 2013–2022 Planetary Science Decadal Survey published in 2011; the proposal envisages launch during 2020–2023 and a 13-year cruise to Uranus.[133] A Uranus entry probe could use Pioneer Venus Multiprobe heritage and descend to 1–5 atmospheres.[133] The ESA evaluated a "medium-class" mission called Uranus Pathfinder.[134] A New Frontiers Uranus Orbiter has been evaluated and recommended in the study, The Case for a Uranus Orbiter.[135] Such a mission is aided by the ease with which a relatively big mass can be sent to the system—over 1500 kg with an Atlas 521 and 12-year journey.[136] For more concepts see Proposed Uranus missions.
In culture
In astrology, the planet Uranus ( ) is the ruling planet of Aquarius. Because Uranus is cyan and Uranus is associated with electricity, the colour electric blue, which is close to cyan, is associated with the sign Aquarius[137] (see Uranus in astrology).
The chemical element uranium, discovered in 1789 by the German chemist Martin Heinrich Klaproth, was named after the newly discovered planet Uranus.[138]
"Uranus, the Magician" is a movement in Gustav Holst's orchestral suite The Planets, written between 1914 and 1916.
Operation Uranus was the successful military operation in World War II by the Soviet army to take back Stalingrad and marked the turning point in the land war against the Wehrmacht.
The lines "Then felt I like some watcher of the skies/When a new planet swims into his ken", from John Keats's "On First Looking Into Chapman's Homer", are a reference to Herschel's discovery of Uranus.[139]
Many references to Uranus in popular culture and news involve humor about one pronunciation of its name resembling that of the phrase "your anus".[140]
See also
Solar System portal
Uranus portal
Book: Uranus
Book: Solar System
Outline of Uranus
2011 QF99 and 2014 YX49, the only two known Uranus trojans
Colonisation of Uranus
Uranus in astrology
Uranus in fiction
Extraterrestrial diamonds (thought to be abundant in Uranus)
Notes
Jump up ^ These are the mean elements from VSOP87, together with derived quantities.
^ Jump up to: a b c d e f g Refers to the level of 1 bar atmospheric pressure.
Jump up ^ Calculated using data from Seidelmann, 2007.[8]
Jump up ^ Based on the volume within the level of 1 bar atmospheric pressure.
Jump up ^ Calculation of He, H2 and CH4 molar fractions is based on a 2.3% mixing ratio of methane to hydrogen and the 15/85 He/H2 proportions measured at the tropopause.
Jump up ^ Because, in the English-speaking world, the latter sounds like "your anus", the former pronunciation also saves embarrassment: as Pamela Gay, an astronomer at Southern Illinois University Edwardsville, noted on her podcast, to avoid "being made fun of by any small schoolchildren ... when in doubt, don't emphasise anything and just say /ˈjʊərənəs/. And then run, quickly."[33]
Jump up ^ Cf. (not supported by all fonts)
Jump up ^ Cf. (not supported by all fonts)
Jump up ^ Mixing ratio is defined as the number of molecules of a compound per a molecule of hydrogen.
References
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Jump up ^ RAS MSS Herschel W1/13.M, 14 quoted in Miner p. 8.
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Further reading
Alexander, Arthur Francis O'Donel (1965). The Planet Uranus – A History of Observation, Theory and Discovery.
Miner, Ellis D. (1998). Uranus: The Planet, Rings and Satellites. New York: John Wiley and Sons. ISBN 978-0-471-97398-0.
Bode, Johann Elert (1784). Von dem neu entdeckten Planeten. Verfasser.
Gore, Rick (August 1986). "Uranus — Voyager Visits a Dark Planet". National Geographic. Vol. 170 no. 2. pp. 178–194. ISSN 0027-9358. OCLC 643483454.
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NASA's Uranus fact sheet
Uranus Profile at NASA's Solar System Exploration site
Planets – Uranus A kid's guide to Uranus.
Uranus at Jet Propulsion Laboratory's planetary photojournal. (photos)
Voyager at Uranus (photos)
Uranus (Astronomy Cast homepage) (blog)
Uranian system montage (photo)
Gray, Meghan; Merrifield, Michael (2010). "Uranus". Sixty Symbols. Brady Haran for the University of Nottingham.
"How to Pronounce Uranus" by CGP Grey
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values: यूरेनस ग्रह – Bhojpuri

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display: none;

values: Уран (планета) – Bulgarian

values:
interlanguage-link interwiki-bg
display: none;

values:
interlanguage-link interwiki-bar
display: none;

values: སྐར་མ་གནམ་རྒྱལ། – Tibetan

values:
interlanguage-link interwiki-bo
display: none;

values:
https://bs.wikipedia.org/wiki/Uran
Uran – Bosnian
bs
bs
interlanguage-link-target

values:
interlanguage-link interwiki-bs
display: none;

values:
interlanguage-link interwiki-br
display: none;

values: Тэнгэриин ван – Russia Buriat

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interlanguage-link interwiki-bxr
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values: Уран (планета) – Chuvash

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interlanguage-link interwiki-cy
display: none;

values:
interlanguage-link interwiki-da
display: none;

values:
https://se.wikipedia.org/wiki/Uranus
Uranus – Northern Sami
se
se
interlanguage-link-target

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display: none;

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interlanguage-link interwiki-de
display: none;

values:
interlanguage-link interwiki-nv
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interlanguage-link interwiki-eml
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interlanguage-link interwiki-eo
display: none;

values:
interlanguage-link interwiki-ext
display: none;

values:
https://eu.wikipedia.org/wiki/Urano
Urano – Basque
eu
eu
interlanguage-link-target

values:
interlanguage-link interwiki-eu
display: none;

values: اورانوس – Persian

values:
interlanguage-link interwiki-fa
display: none;

values:
https://hif.wikipedia.org/wiki/Arungrah
Arungrah – Fiji Hindi
hif
hif
interlanguage-link-target

values:
interlanguage-link interwiki-hif
display: none;

values:
https://fo.wikipedia.org/wiki/Uranus
Uranus – Faroese
fo
fo
interlanguage-link-target

values:
interlanguage-link interwiki-fo
display: none;

values:
interlanguage-link interwiki-fr
display: none;

values:
https://fy.wikipedia.org/wiki/Uranus
Uranus – Western Frisian
fy
fy
interlanguage-link-target

values:
interlanguage-link interwiki-fy
display: none;

values:
interlanguage-link interwiki-ga
display: none;

values:
https://gv.wikipedia.org/wiki/Uraanus
Uraanus – Manx
gv
gv
interlanguage-link-target

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interlanguage-link interwiki-gv
display: none;

values:
interlanguage-link interwiki-gd
display: none;

values:
https://gl.wikipedia.org/wiki/Urano
Urano – Galician
gl
gl
interlanguage-link-target

values:
interlanguage-link interwiki-gl
display: none;

values:
interlanguage-link interwiki-gan
display: none;

values: યુરેનસ (ગ્રહ) – Gujarati

values:
interlanguage-link interwiki-gu
display: none;

values:
interlanguage-link interwiki-hak
display: none;

values:
interlanguage-link interwiki-ko
display: none;

values:
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values: Ուրան (մոլորակ) – Armenian

values: interlanguage-link interwiki-hy badge-Q17437798 badge-goodarticle

values: अरुण (ग्रह) – Hindi

values:
interlanguage-link interwiki-hi
display: none;

values:
https://hr.wikipedia.org/wiki/Uran
Uran – Croatian
hr
hr
interlanguage-link-target

values:
interlanguage-link interwiki-hr
display: none;

values:
https://io.wikipedia.org/wiki/Urano
Urano – Ido
io
io
interlanguage-link-target

values:
interlanguage-link interwiki-io
display: none;

values:
https://ilo.wikipedia.org/wiki/Urano
Urano – Iloko
ilo
ilo
interlanguage-link-target

values:
interlanguage-link interwiki-ilo
display: none;

values:
https://id.wikipedia.org/wiki/Uranus
Uranus – Indonesian
id
id
interlanguage-link-target

values:
interlanguage-link interwiki-id
display: none;

values:
https://ia.wikipedia.org/wiki/Urano
Urano – Interlingua
ia
ia
interlanguage-link-target

values:
interlanguage-link interwiki-ia
display: none;

values:
interlanguage-link interwiki-iu
display: none;

values: Уран (планетæ) – Ossetic

values:
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display: none;

values:
https://zu.wikipedia.org/wiki/UYurenasi
UYurenasi – Zulu
zu
zu
interlanguage-link-target

values:
interlanguage-link interwiki-zu
display: none;

values:
interlanguage-link interwiki-is
display: none;

values:
interlanguage-link interwiki-it
display: none;

values: אורנוס – Hebrew

values:
interlanguage-link interwiki-he
display: none;

values:
https://jv.wikipedia.org/wiki/Uranus
Uranus – Javanese
jv
jv
interlanguage-link-target

values:
interlanguage-link interwiki-jv
display: none;

values: ಯುರೇನಸ್ – Kannada

values:
interlanguage-link interwiki-kn
display: none;

values:
https://pam.wikipedia.org/wiki/Uranus
Uranus – Pampanga
pam
pam
interlanguage-link-target

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display: none;

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values: Уран (ғаламшар) – Kazakh

values:
interlanguage-link interwiki-kk
display: none;

values:
interlanguage-link interwiki-kw
display: none;

values:
https://sw.wikipedia.org/wiki/Uranus
Uranus – Swahili
sw
sw
interlanguage-link-target

values:
interlanguage-link interwiki-sw
display: none;

values: Уран (планет) – Komi

values:
interlanguage-link interwiki-kv
display: none;

values:
https://kg.wikipedia.org/wiki/Uranus
Uranus – Kongo
kg
kg
interlanguage-link-target

values:
interlanguage-link interwiki-kg
display: none;

values:
https://ht.wikipedia.org/wiki/Iranis
Iranis – Haitian Creole
ht
ht
interlanguage-link-target

values:
interlanguage-link interwiki-ht
display: none;

values:
interlanguage-link interwiki-ku
display: none;

values: Уран (планета) – Kyrgyz

values:
interlanguage-link interwiki-ky
display: none;

values: Уран (планета) – Lezghian

values:
interlanguage-link interwiki-lez
display: none;

values: ດາວຢູລານຸດ – Lao

values:
interlanguage-link interwiki-lo
display: none;

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values:
interlanguage-link interwiki-lt
display: none;

values:
interlanguage-link interwiki-lij
display: none;

values:
interlanguage-link interwiki-li
display: none;

values:
https://olo.wikipedia.org/wiki/Uranus
Uranus – Livvi-Karelian
olo
olo
interlanguage-link-target

values:
interlanguage-link interwiki-olo
display: none;

values:
https://jbo.wikipedia.org/wiki/uranos
uranos – Lojban
jbo
jbo
interlanguage-link-target

values:
interlanguage-link interwiki-jbo
display: none;

values:
interlanguage-link interwiki-lmo
display: none;

values:
interlanguage-link interwiki-hu
display: none;

values: अरुण ग्रह – Maithili

values:
interlanguage-link interwiki-mai
display: none;

values: Уран (планета) – Macedonian

values:
interlanguage-link interwiki-mk
display: none;

values:
https://mg.wikipedia.org/wiki/Uranus
Uranus – Malagasy
mg
mg
interlanguage-link-target

values:
interlanguage-link interwiki-mg
display: none;

values:
interlanguage-link interwiki-ml
display: none;

values:
interlanguage-link interwiki-mt
display: none;

values: युरेनस ग्रह – Marathi

values:
interlanguage-link interwiki-mr
display: none;

values: ურანი (პლანეტა) – Mingrelian

values:
interlanguage-link interwiki-xmf
display: none;

values:
interlanguage-link interwiki-arz
display: none;

values:
interlanguage-link interwiki-mzn
display: none;

values:
https://ms.wikipedia.org/wiki/Uranus
Uranus – Malay
ms
ms
interlanguage-link-target

values:
interlanguage-link interwiki-ms
display: none;

values:
interlanguage-link interwiki-cdo
display: none;

values:
https://mwl.wikipedia.org/wiki/Ourano
Ourano – Mirandese
mwl
mwl
interlanguage-link-target

values:
interlanguage-link interwiki-mwl
display: none;

values: Уран (шары тяште) – Moksha

values:
interlanguage-link interwiki-mdf
display: none;

values: Тэнгэрийн ван – Mongolian

values:
interlanguage-link interwiki-mn
display: none;

values: ယူရေးနပ်စ်ဂြိုဟ် – Burmese

values:
interlanguage-link interwiki-my
display: none;

values:
interlanguage-link interwiki-nah
display: none;

values:
interlanguage-link interwiki-nl
display: none;

values:
interlanguage-link interwiki-nds-nl
display: none;

values: अरुणग्रह – Nepali

values:
interlanguage-link interwiki-ne
display: none;

values:
interlanguage-link interwiki-ja
display: none;

values:
https://nap.wikipedia.org/wiki/Urano
Urano – Neapolitan
nap
nap
interlanguage-link-target

values:
interlanguage-link interwiki-nap
display: none;

values:
interlanguage-link interwiki-ce
display: none;

values:
https://frr.wikipedia.org/wiki/Uranus
Uranus – Northern Frisian
frr
frr
interlanguage-link-target

values:
interlanguage-link interwiki-frr
display: none;

values:
https://no.wikipedia.org/wiki/Uranus
Uranus – Norwegian
no
no
interlanguage-link-target

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values:
interlanguage-link interwiki-nn
display: none;

values:
interlanguage-link interwiki-nov
display: none;

values: interlanguage-link interwiki-oc badge-Q17437796 badge-featuredarticle

values: ଇଉରେନ୍ସେ – Odia

values:
interlanguage-link interwiki-or
display: none;

values:
interlanguage-link interwiki-uz
display: none;

values: ਯੁਰੇਨਸ (ਗ੍ਰਹਿ) – Punjabi

values:
interlanguage-link interwiki-pa
display: none;

values:
interlanguage-link interwiki-pnb
display: none;

values: اورانوس – Pashto

values:
interlanguage-link interwiki-ps
display: none;

values:
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display: none;

values: ភពអ៊ុយរ៉ានុស – Khmer

values:
interlanguage-link interwiki-km
display: none;

values:
interlanguage-link interwiki-pms
display: none;

values:
interlanguage-link interwiki-tpi
display: none;

values:
interlanguage-link interwiki-nds
display: none;

values:
https://pl.wikipedia.org/wiki/Uran
Uran – Polish
pl
pl
interlanguage-link-target

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values:
interlanguage-link interwiki-kaa
display: none;

values:
interlanguage-link interwiki-ksh
display: none;

values:
https://ro.wikipedia.org/wiki/Uranus
Uranus – Romanian
ro
ro
interlanguage-link-target

values:
interlanguage-link interwiki-ro
display: none;

values:
https://rmy.wikipedia.org/wiki/Rahor
Rahor – Romani
rmy
rmy
interlanguage-link-target

values:
interlanguage-link interwiki-rmy
display: none;

values:
interlanguage-link interwiki-rm
display: none;

values:
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display: none;

values: Уран (планета) – Rusyn

values:
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display: none;

values: Уран (планета) – Russian

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values: Ураан (планета) – Sakha

values:
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display: none;

values: युरेनस्-ग्रहः – Sanskrit

values:
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display: none;

values:
https://sc.wikipedia.org/wiki/Uranu
Uranu – Sardinian
sc
sc
interlanguage-link-target

values:
interlanguage-link interwiki-sc
display: none;

values:
https://sco.wikipedia.org/wiki/Uranus
Uranus – Scots
sco
sco
interlanguage-link-target

values:
interlanguage-link interwiki-sco
display: none;

values:
https://stq.wikipedia.org/wiki/Uranus
Uranus – Saterland Frisian
stq
stq
interlanguage-link-target

values:
interlanguage-link interwiki-stq
display: none;

values:
https://st.wikipedia.org/wiki/Yuranese
Yuranese – Southern Sotho
st
st
interlanguage-link-target

values:
interlanguage-link interwiki-st
display: none;

values:
interlanguage-link interwiki-sq
display: none;

values:
interlanguage-link interwiki-scn
display: none;

values: යු‍රේනස් – Sinhala

values:
interlanguage-link interwiki-si
display: none;

values:
interlanguage-link interwiki-simple
display: none;

values: يورينس – Sindhi

values:
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display: none;

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values:
interlanguage-link interwiki-sl
display: none;

values:
interlanguage-link interwiki-szl
display: none;

values:
https://so.wikipedia.org/wiki/Uraano
Uraano – Somali
so
so
interlanguage-link-target

values:
interlanguage-link interwiki-so
display: none;

values:
interlanguage-link interwiki-ckb
display: none;

values:
interlanguage-link interwiki-sr
display: none;

values:
interlanguage-link interwiki-sh
display: none;

values:
https://su.wikipedia.org/wiki/Uranus
Uranus – Sundanese
su
su
interlanguage-link-target

values:
interlanguage-link interwiki-su
display: none;

values:
https://fi.wikipedia.org/wiki/Uranus
Uranus – Finnish
fi
fi
interlanguage-link-target

values:
interlanguage-link interwiki-fi
display: none;

values:
https://sv.wikipedia.org/wiki/Uranus
Uranus – Swedish
sv
sv
interlanguage-link-target

values:
interlanguage-link interwiki-sv
display: none;

values:
https://tl.wikipedia.org/wiki/Urano
Urano – Tagalog
tl
tl
interlanguage-link-target

values:
interlanguage-link interwiki-tl
display: none;

values: யுரேனசு – Tamil

values:
interlanguage-link interwiki-ta
display: none;

values: Уран (планета) – Tatar

values:
interlanguage-link interwiki-tt
display: none;

values: యురేనస్ – Telugu

values:
interlanguage-link interwiki-te
display: none;

values: ดาวยูเรนัส – Thai

values:
interlanguage-link interwiki-th
display: none;

values: Уран (сайёра) – Tajik

values:
interlanguage-link interwiki-tg
display: none;

values:
interlanguage-link interwiki-chr
display: none;

values:
interlanguage-link interwiki-tr
display: none;

values:
interlanguage-link interwiki-tk
display: none;

values:
interlanguage-link interwiki-tyv
display: none;

values: Уран (планета) – Ukrainian

values:
interlanguage-link interwiki-uk
display: none;

values: یورینس – Urdu

values:
interlanguage-link interwiki-ur
display: none;

values: ئۇران (پلانىت) – Uyghur

values:
interlanguage-link interwiki-ug
display: none;

values:
interlanguage-link interwiki-za
display: none;

values:
interlanguage-link interwiki-vep
display: none;

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values:
https://vo.wikipedia.org/wiki/Uranud
Uranud – Volapük
vo
vo
interlanguage-link-target

values:
interlanguage-link interwiki-vo
display: none;

values:
interlanguage-link interwiki-fiu-vro
display: none;

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values:
https://vls.wikipedia.org/wiki/Uranus
Uranus – West Flemish
vls
vls
interlanguage-link-target

values:
interlanguage-link interwiki-vls
display: none;

values:
https://war.wikipedia.org/wiki/Urano
Urano – Waray
war
war
interlanguage-link-target

values:
interlanguage-link interwiki-war
display: none;

values:
https://wo.wikipedia.org/wiki/Uraanus
Uraanus – Wolof
wo
wo
interlanguage-link-target

values:
interlanguage-link interwiki-wo
display: none;

values:
interlanguage-link interwiki-wuu
display: none;

values: אוראנוס – Yiddish

values:
interlanguage-link interwiki-yi
display: none;

values:
interlanguage-link interwiki-yo
display: none;

values:
interlanguage-link interwiki-zh-yue
display: none;

values:
https://diq.wikipedia.org/wiki/Uranus
Uranus – Zazaki
diq
diq
interlanguage-link-target

values:
interlanguage-link interwiki-diq
display: none;

values:
interlanguage-link interwiki-zea
display: none;

values:
interlanguage-link interwiki-bat-smg
display: none;

values: interlanguage-link interwiki-zh badge-Q17437798 badge-goodarticle

values: अरुणग्रह – Doteli

values:
interlanguage-link interwiki-dty
display: none;

values:
https://kbp.wikipedia.org/wiki/Uranisi
Uranisi – Kabiye
kbp
kbp
interlanguage-link-target

values:
interlanguage-link interwiki-kbp
display: none;

values: All languages (initial selection from common choices by you and others)

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display: none; font-size: 13px;

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