Astronomy:Moons of Uranus

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Short description: Natural satellites of the planet Uranus

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An updated image of the six largest moons and eight inner moons of Uranus as captured by the James Webb Space Telescope on September 4, 2023. The six largest moons are Ariel, Puck, Miranda, Umbriel, Titania and Oberon. Unlike the previous image taken on February 6, 2023, eight additional small moons can now be seen, including Bianca, Cressida, Desdemona, Juliet, Portia, Rosalind, Belinda and Perdita. Cordelia and Ophelia are invisible because they are lost in the overpowering brightness of the Epsilon ring, while Mab and Cupid are too small to be seen.

Uranus, the seventh planet of the Solar System, has at least 27 moons, most of which are named after characters that appear in, or are mentioned in, the works of William Shakespeare and Alexander Pope.[1] Uranus' moons are divided into three groups: thirteen inner moons, five major moons, and nine irregular moons. The inner and major moons all have prograde orbits, while orbits of the irregulars are mostly retrograde.

The inner moons are small dark bodies that share common properties and origins with Uranus's rings. The five major moons are ellipsoidal, indicating that they reached hydrostatic equilibrium at some point in their past (and may still be in equilibrium), and four of them show signs of internally driven processes such as canyon formation and volcanism on their surfaces.[2] The largest of these five, Titania, is 1,578 km in diameter and the eighth-largest moon in the Solar System, about one-twentieth the mass of the Earth's Moon. The orbits of the regular moons are nearly coplanar with Uranus's equator, which is tilted 97.77° to its orbit. Uranus's irregular moons have elliptical and strongly inclined (mostly retrograde) orbits at large distances from the planet.[3]

William Herschel discovered the first two moons, Titania and Oberon, in 1787. The other three ellipsoidal moons were discovered in 1851 by William Lassell (Ariel and Umbriel) and in 1948 by Gerard Kuiper (Miranda).[1] These five may be in hydrostatic equilibrium, and so would be considered dwarf planets if they were in direct orbit about the Sun. The remaining moons were discovered after 1985, either during the Voyager 2 flyby mission or with the aid of advanced Earth-based telescopes.[2][3]

Discovery

The first two moons to be discovered were Titania and Oberon, which were spotted by Sir William Herschel on January 11, 1787, six years after he had discovered the planet itself. Later, Herschel thought he had discovered up to six moons (see below) and perhaps even a ring. For nearly 50 years, Herschel's instrument was the only one with which the moons had been seen.[4] In the 1840s, better instruments and a more favorable position of Uranus in the sky led to sporadic indications of satellites additional to Titania and Oberon. Eventually, the next two moons, Ariel and Umbriel, were discovered by William Lassell in 1851.[5] The Roman numbering scheme of Uranus's moons was in a state of flux for a considerable time, and publications hesitated between Herschel's designations (where Titania and Oberon are Uranus II and IV) and William Lassell's (where they are sometimes I and II).[6] With the confirmation of Ariel and Umbriel, Lassell numbered the moons I through IV from Uranus outward, and this finally stuck.[7] In 1852, Herschel's son John Herschel gave the four then-known moons their names.[8]

No other discoveries were made for almost another century. In 1948, Gerard Kuiper at the McDonald Observatory discovered the smallest and the last of the five large, spherical moons, Miranda.[8][9] Decades later, the flyby of the Voyager 2 space probe in January 1986 led to the discovery of ten further inner moons.[2] Another satellite, Perdita, was discovered in 1999[10] after studying old Voyager photographs.[11]

Uranus was the last giant planet without any known irregular moons, but since 1997 nine distant irregular moons have been identified using ground-based telescopes.[3] Two more small inner moons, Cupid and Mab, were discovered using the Hubble Space Telescope in 2003.[12] As of 2020, the moon Margaret was the last Uranian moon discovered, and its characteristics were published in October 2003.[13]

Spurious moons

After Herschel discovered Titania and Oberon on January 11, 1787, he subsequently believed that he had observed four other moons: two on January 18 and February 9, 1790, and two more on February 28 and March 26, 1794. It was thus believed for many decades thereafter that Uranus had a system of six satellites, though the four latter moons were never confirmed by any other astronomer. Lassell's observations of 1851, in which he discovered Ariel and Umbriel, however, failed to support Herschel's observations; Ariel and Umbriel, which Herschel certainly ought to have seen if he had seen any satellites beside Titania and Oberon, did not correspond to any of Herschel's four additional satellites in orbital characteristics. Herschel's four spurious satellites were thought to have sidereal periods of 5.89 days (interior to Titania), 10.96 days (between Titania and Oberon), 38.08 days, and 107.69 days (exterior to Oberon).[14] It was therefore concluded that Herschel's four satellites were spurious, probably arising from the misidentification of faint stars in the vicinity of Uranus as satellites, and the credit for the discovery of Ariel and Umbriel was given to Lassell.[15]


Names

Main page: Astronomy:Naming of moons

Although the first two Uranian moons were discovered in 1787, they were not named until 1852, a year after two more moons had been discovered. The responsibility for naming was taken by John Herschel, son of the discoverer of Uranus. Herschel, instead of assigning names from Greek mythology, named the moons after magical spirits in English literature: the fairies Oberon and Titania from William Shakespeare's A Midsummer Night's Dream, and the sylph Ariel and gnome Umbriel from Alexander Pope's The Rape of the Lock (Ariel is also a sprite in Shakespeare's The Tempest). The reasoning was presumably that Uranus, as god of the sky and air, would be attended by spirits of the air.[16]

Subsequent names, rather than continuing the airy spirits theme (only Puck and Mab continued the trend), have focused on Herschel's source material. In 1949, the fifth moon, Miranda, was named by its discoverer Gerard Kuiper after a thoroughly mortal character in Shakespeare's The Tempest. The current IAU practice is to name moons after characters from Shakespeare's plays and The Rape of the Lock (although at present only Ariel, Umbriel, and Belinda have names drawn from the latter; all the rest are from Shakespeare). The outer retrograde moons are all named after characters from one play, The Tempest; the sole known outer prograde moon, Margaret, is named from Much Ado About Nothing.[8]

Some asteroids, also named after the same Shakespearean characters, share names with moons of Uranus: 171 Ophelia, 218 Bianca, 593 Titania, 666 Desdemona, 763 Cupido, and 2758 Cordelia.

Characteristics and groups

The Uranian satellite system is the least massive among those of the giant planets. Indeed, the combined mass of the five major satellites is less than half that of Triton (the seventh-largest moon in the Solar System) alone.[lower-alpha 1] The largest of the satellites, Titania, has a radius of 788.9 km,[18] or less than half that of the Moon, but slightly more than that of Rhea, the second-largest moon of Saturn, making Titania the eighth-largest moon in the Solar System. Uranus is about 10,000 times more massive than its moons.[lower-alpha 2]

Inner moons

Schematic of the Uranian moon–ring system

As of 2020, Uranus is known to have 13 inner moons.[12] Their orbits lie inside that of Miranda. All of the inner moons are intimately connected with the rings of Uranus, which probably resulted from the fragmentation of one or several small inner moons.[19] The two innermost moons (Cordelia and Ophelia) are shepherds of Uranus's ε ring, whereas the small moon Mab is a source of Uranus's outermost μ ring.[12] There may be two additional small (2–7 km in radius) undiscovered shepherd moons located about 100 km exterior to Uranus's α and β rings.[20]

At 162 km, Puck is the largest of the inner moons of Uranus and the only one imaged by Voyager 2 in any detail. Puck and Mab are the two outermost inner satellites of Uranus. All inner moons are dark objects; their geometrical albedo is less than 10%.[21] They are composed of water ice contaminated with a dark material, probably radiation-processed organics.[22]

The small inner moons constantly perturb each other. The system is chaotic and apparently unstable.[23] Simulations show that the moons may perturb each other into crossing orbits, which may eventually result in collisions between the moons.[12] Desdemona may collide with Cressida within the next million years,[24] and Cupid will likely collide with Belinda in the next 10 million years; Perdita and Juliet may be involved in later collisions.[25] Because of this, the rings and inner moons may be under constant flux, with moons colliding and re-accreting on short timescales.[25]

Large moons

Uranus and its six largest moons compared at their proper relative sizes and in the correct order. From left to right: Puck, Miranda, Ariel, Umbriel, Titania, and Oberon

Uranus has five major moons: Miranda, Ariel, Umbriel, Titania, and Oberon. They range in diameter from 472 km for Miranda to 1578 km for Titania.[18] All these moons are relatively dark objects: their geometrical albedo varies between 30 and 50%, whereas their Bond albedo is between 10 and 23%.[21] Umbriel is the darkest moon and Ariel the brightest. The masses of the moons range from 6.7 × 1019 kg (Miranda) to 3.5 × 1021 kg (Titania). For comparison, the Moon has a mass of 7.5 × 1022 kg.[26] The major moons of Uranus are thought to have formed in the accretion disc, which existed around Uranus for some time after its formation or resulted from a large impact suffered by Uranus early in its history.[27][28] This view is supported by their large thermal inertia, a surface property they share with dwarf planets like Pluto and Haumea.[29] It differs strongly from the thermal behaviour of the Uranian irregular moons that is comparable to classical trans-Neptunian objects.[30] This suggests a separate origin.

Moons (Ariel, Umbriel, Titania, Oberon, Miranda)
Modeling (4 May 2023)

All major moons comprise approximately equal amounts rock and ice, except Miranda, which is made primarily of ice.[31] The ice component may include ammonia and carbon dioxide.[32] Their surfaces are heavily cratered, though all of them (except Umbriel) show signs of endogenic resurfacing in the form of lineaments (canyons) and, in the case of Miranda, ovoid race-track like structures called coronae.[2] Extensional processes associated with upwelling diapirs are likely responsible for the origin of the coronae.[33] Ariel appears to have the youngest surface with the fewest impact craters, while Umbriel's appears oldest.[2] A past 3:1 orbital resonance between Miranda and Umbriel and a past 4:1 resonance between Ariel and Titania are thought to be responsible for the heating that caused substantial endogenic activity on Miranda and Ariel.[34][35] One piece of evidence for such a past resonance is Miranda's unusually high orbital inclination (4.34°) for a body so close to the planet.[36][37] The largest Uranian moons may be internally differentiated, with rocky cores at their centers surrounded by ice mantles.[31] Titania and Oberon may harbor liquid water oceans at the core/mantle boundary.[31] The major moons of Uranus are airless bodies. For instance, Titania was shown to possess no atmosphere at a pressure larger than 10–20 nanobar.[38]

The path of the Sun in the local sky over the course of a local day during Uranus's and its major moons' summer solstice is quite different from that seen on most other Solar System worlds. The major moons have almost exactly the same rotational axial tilt as Uranus (their axes are parallel to that of Uranus).[2] The Sun would appear to follow a circular path around Uranus's celestial pole in the sky, at the closest about 7 degrees from it,[lower-alpha 3] during the hemispheric summer. Near the equator, it would be seen nearly due north or due south (depending on the season). At latitudes higher than 7°, the Sun would trace a circular path about 15 degrees in diameter in the sky, and never set during the hermispheric summer, moving to a position over the celestial equator during the Uranian equinox, and then invisible below the horizon during the hemispheric winter.

Irregular moons

See also: Irregular moon
Irregular moons of Uranus. The X axis is labeled in Gm (million km) and in the fraction of the Hill sphere's radius. The eccentricity is represented by the yellow segments (extending from the pericentre to the apocentre) with the inclination represented on the Y axis.
As of 2005 Uranus is known to have nine irregular moons, which orbit it at a distance much greater than that of Oberon, the furthest of the large moons. All the irregular moons are probably captured objects that were trapped by Uranus soon after its formation.[3] The diagram illustrates the orbits of those irregular moons discovered so far. The moons above the X axis are prograde, those beneath are retrograde. The radius of the Uranian Hill sphere is approximately 73 million km.[3]

Uranus's irregular moons range in size from 120–200 km (Sycorax) to about 20 km (Trinculo).[3] Unlike Jupiter's irregulars, Uranus's show no correlation of axis with inclination. Instead, the retrograde moons can be divided into two groups based on axis/orbital eccentricity. The inner group includes those satellites closer to Uranus (a < 0.15 rH) and moderately eccentric (~0.2), namely Francisco, Caliban, Stephano, and Trinculo.[3] The outer group (a > 0.15 rH) includes satellites with high eccentricity (~0.5): Sycorax, Prospero, Setebos, and Ferdinand.[3]

The intermediate inclinations 60° < i < 140° are devoid of known moons due to the Kozai instability.[3] In this instability region, solar perturbations at apoapse cause the moons to acquire large eccentricities that lead to collisions with inner satellites or ejection. The lifetime of moons in the instability region is from 10 million to a billion years.[3]

Margaret is the only known irregular prograde moon of Uranus, and it currently has the most eccentric orbit of any moon in the Solar System, though Neptune's moon Nereid has a higher mean eccentricity. As of 2008, Margaret's eccentricity is 0.7979.[39]

List

Orbital diagram of the orbital inclination and orbital distances for Uranus's rings and moon system at various scales. Notable moons and rings are individually labeled. Open the image for full resolution.
Key
¡
Inner moons
  		†
Major moons
  		‡
Irregular moons (retrograde) 		±
Irregular moon (prograde)

The Uranian moons are listed here by orbital period, from shortest to longest. Moons massive enough for their surfaces to have collapsed into a spheroid are highlighted in light blue and bolded. The inner and major moons all have prograde orbits. Irregular moons with retrograde orbits are shown in dark grey. Margaret, the only known irregular moon of Uranus with a prograde orbit, is shown in light grey. The orbits and mean distances of the irregular moons are variable over short timescales due to frequent planetary and solar perturbations, therefore the listed orbital elements of all irregular moons are averaged over a 8,000-year numerical integration by Brozović and Jacobson (2009). These may differ from osculating orbital elements provided by other sources.[40] Their orbital elements are all based on the epoch of 1 January 2000 Terrestrial Time.[41]

Uranian moons
Label
[lower-alpha 4] 		Name Pronunciation
(key) 		Named after[1] Image Abs.
magn. 		Diameter
(km)[lower-alpha 5] 		Mass
(× 1016 kg)[lower-alpha 6] 		Semi-major axis
(km)[41] 		Orbital period
(d)[41][lower-alpha 7] 		Inclination
(°)[41][lower-alpha 8] 		Eccentricity
[43] 		Discovery
year[1] 		Discoverer
[1]
06 VI ¡Cordelia /kɔːrˈdiːliə/ Daughter of Lear in King Lear Cordeliamoon.png 10.3 0040 40 ± 6
(50 × 36) 		000004 ≈ 4.4 00049000 49770 0000.33 +0.33503 000.084 0.08479° 0.00026 1986 Terrile
(Voyager 2)
07 VII ¡Ophelia /oʊˈfiːliə/ Daughter of Polonius and fiancée of Hamlet in Hamlet Opheliamoon.png 10.2 0043 43 ± 8
(54 × 38) 		000005 ≈ 5.3 00053000 53790 0000.37 +0.37640 000.103 0.1036° 0.00992 1986 Terrile
(Voyager 2)
08 VIII ¡Bianca /biˈɑːŋkə/ Daughter of Baptista in The Taming of the Shrew Biancamoon.png 9.8 0051 51 ± 4
(64 × 46) 		000009 ≈ 9.2 00059000 59170 0000.43 +0.43458 000.193 0.193° 0.00092 1986 Smith
(Voyager 2)
09 IX ¡Cressida /ˈkrɛsədə/ Cressida, female protagonist of Troilus and Cressida Cressida.png 8.9 0080 80 ± 4
(92 × 74) 		000034 ≈ 34 00061000 61780 0000.46 +0.46357 000.006 0.006° 0.00036 1986 Synnott
(Voyager 2)
10 X ¡Desdemona /ˌdɛzdəˈmoʊnə/ Wife of Othello in Othello Desdemonamoon.png 9.3 0064 64 ± 8
(90 × 54) 		000018 ≈ 18 00062000 62680 0000.47 +0.47365 000.111 0.11125° 0.00013 1986 Synnott
(Voyager 2)
11 XI ¡Juliet /ˈdʒuːliət/ Female protagonist of Romeo and Juliet Julietmoon.png 8.5 0094 94 ± 8
(150 × 74) 		000056 ≈ 56 00064000 64350 0000.49 +0.49307 000.065 0.065° 0.00066 1986 Synnott
(Voyager 2)
12 XII ¡Portia /ˈpɔːrʃə/ Portia, the beautiful, intelligent and rich heiress of Belmont in The Merchant of Venice Portia1.jpg 7.7 0135 135 ± 8
(156 × 126) 		000170 ≈ 170 00066000 66090 0000.51 +0.51320 000.059 0.059° 0.00005 1986 Synnott
(Voyager 2)
13 XIII ¡Rosalind /ˈrɒzələnd/ Daughter of the banished duke in As You Like It Rosalindmoon.png 9.1 0072 72 ± 12 000025 ≈ 25 00069000 69940 0000.55 +0.55846 000.279 0.279° 0.00011 1986 Synnott
(Voyager 2)
27 XXVII ¡Cupid /ˈkjuːpəd/ Minor character in Timon of Athens Cupidmoon.png 12.6 0018 ≈ 18 000000.38 ≈ 0.38 00074000 74800 0000.61 +0.61800 000.100 0.100° 0.0013 2003 Showalter and
Lissauer
14 XIV ¡Belinda /bəˈlɪndə/ Protagonist of The Rape of the Lock
Belinda.gif
 8.8 0090 90 ± 16
(128 × 64) 		000049 ≈ 49 00075000 75260 0000.62 +0.62353 000.031 0.031° 0.00007 1986 Synnott
(Voyager 2)
25 XXV ¡Perdita /ˈpɜːrdətə/ Daughter of Leontes and Hermione in The Winter's Tale Perditamoon.png 11.0 0030 30 ± 6 000002 ≈ 1.8 00076000 76400 0000.63 +0.63800 000 0.0° 0.0012 1999 Karkoschka
(Voyager 2)
15 XV ¡Puck /ˈpʌk/ Puck, a mischievous spirit in A Midsummer Night's Dream
Puck.png
 7.3 0162 162 ± 4 000290 ≈ 290 00086000 86010 0000.76 +0.76183 000.319 0.3192° 0.00012 1985 Synnott
(Voyager 2)
26 XXVI ¡Mab /ˈmæb/ Midwife of the fairies in Romeo and Juliet
Mabmoon.png
 12.1 0018 ≈ 18 000000.38 ≈ 0.38 00097000 97700 0000.92 +0.92300 000.133 0.1335° 0.0025 2003 Showalter and
Lissauer
05 V †Miranda /məˈrændə/ Miranda, lead character in The Tempest
Miranda - January 24 1986 (30906319004).jpg
 3.5 0470 471.6 ± 1.4
(481 × 468 × 466) 		006600 6400±300 00129000 129390 0001.4 +1.41348 004 4.232° 0.0013 1948 Kuiper
01 I †Ariel /ˈɛəriɛl/ Sylph (a type of air spirit) in The Rape of the Lock
Ariel (moon).jpg
 1.0 1157 1157.8±1.2
(1162 × 1156 × 1155) 		125000 125100±2100 00191000 191020 0002.5 +2.52038 000.260 0.260° 0.0012 1851 Lassell
02 II †Umbriel /ˈʌmbriəl/ Evil spirit in The Rape of the Lock
PIA00040 Umbrielx2.47.jpg
 1.7 1169 1169.4±5.6 127000 127500±2800 00266000 266300 0004.1 +4.14418 000.205 0.205° 0.0039 1851 Lassell
03 III †Titania /təˈtɑːniə/ Queen of the fairies in A Midsummer Night's Dream
Titania (moon) color, cropped.jpg
 0.8 1577 1576.8±1.2 340000 340000±6100 00435000 435910 0008.7 +8.70587 000.340 0.340° 0.0011 1787 Herschel
04 IV †Oberon /ˈoʊbərɒn/ King of the fairies in A Midsummer Night's Dream
Voyager 2 picture of Oberon.jpg
 1.0 1522 1522.8±5.2 301000 307600±8700 00583000 583520 0013 +13.4632 000.058 0.058° 0.0014 1787 Herschel
22 XXII ‡Francisco /frænˈsɪskoʊ/ Lord in The Tempest 12.4 0022 ≈ 22 000000.72 ≈ 0.72 04282900 4282900 0267 −267.09 147.250° 0.1324 2003[lower-alpha 9] Holman et al.
16 XVI ‡Caliban /ˈkælɪbæn/ Caliban, the monstrous slave in The Tempest Caliban discovery.jpg 9.1 0042 42+20
−12 		000025 ≈ 25 07231100 7231100 0579 −579.73 141.529° 0.1812 1997 Gladman et al.
20 XX ‡Stephano /ˈstɛfənoʊ/ Drunken butler in The Tempest Stephano - Uranus moon.jpg 9.7 0032 ≈ 32 000002.2 ≈ 2.2 08007400 8007400 0677 −677.47 143.819° 0.2248 1999 Gladman et al.
21 XXI ‡Trinculo /ˈtrɪŋkjʊloʊ/ Jester in The Tempest 12.7 0018 ≈ 18 000000.39 ≈ 0.39 08505200 8505200 0749 −749.40 166.971° 0.2194 2001 Holman et al.
17 XVII ‡Sycorax /ˈsɪkəræks/ Mother of Caliban in The Tempest Sycorax.jpg 7.4 0157 157+23
−15 		000230 ≈ 230 12179400 12179400 1288 −1288.38 159.420° 0.5219 1997 Nicholson et al.
23 XXIII ±Margaret /ˈmɑːrɡərət/ Gentlewoman attending on Hero in Much Ado About Nothing S2003u3acircle.gif 12.7 0020 ≈ 20 000000.54 ≈ 0.54 14146700 14146700 1661 +1661.00 57.367° 0.6772 2003 Sheppard and
Jewitt
18 XVIII ‡Prospero /ˈprɒspəroʊ/ Rightful Duke of Milan in The Tempest Prospero - Uranus moon.jpg 10.5 0050 ≈ 50 000008.5 ≈ 8.5 16276800 16276800 1978 −1978.37 151.830° 0.4445 1999 Holman et al.
19 XIX ‡Setebos /ˈsɛtɛbʌs/ Deity worshipped by Sycorax in The Tempest Uranus - Setebos image.jpg 10.7 0048 ≈ 48 000007.5 ≈ 7.5 17420400 17420400 2225 −2225.08 158.235° 0.5908 1999 Kavelaars et al.
24 XXIV ‡Ferdinand /ˈfɜːrdənænd/ Son of the King of Naples in The Tempest Uranus moon 021002 02.jpg 12.5 0012 ≈ 12 000000.54 ≈ 0.54 20430000 20430000 2790 −2790.03 169.793° 0.3993 2003[lower-alpha 9] Holman et al.

Sources: NASA/NSSDC,[41] Sheppard, et al. 2005.[3] For the recently discovered outer irregular moons (Francisco through Ferdinand) the most accurate orbital data can be generated with the Minor Planet Center's Natural Satellites Ephemeris Service.[39] The irregulars are significantly perturbed by the Sun.[3]

See also

Notes

  1. ↑ The mass of Triton is about 2.14 × 1022 kg,[17] whereas the combined mass of the Uranian moons is about 0.92 × 1022 kg.
  2. ↑ Uranus mass of 8.681 × 1025 kg / Mass of Uranian moons of 0.93 × 1022 kg
  3. ↑ The axial tilt of Uranus is 97°.[2]
  4. ↑ Label refers to the Roman numeral attributed to each moon in order of their discovery.[1]
  5. ↑ Diameters with multiple entries such as "60 × 40 × 34" reflect that the body is not a perfect spheroid and that each of its dimensions have been measured well enough. The diameters and dimensions of Miranda, Ariel, Umbriel, and Oberon were taken from Thomas, 1988.[18] The diameter of Titania is from Widemann, 2009.[38] The dimensions and radii of the inner moons are from Karkoschka, 2001,[11] except for Cupid and Mab, which were taken from Showalter, 2006.[12] The radii of outer moons except Sycorax and Caliban were taken from Sheppard, 2005.[3] The radii of Sycorax and Caliban are from Farkas-Takács et al., 2017.[42]
  6. ↑ Masses of Miranda, Ariel, Umbriel, Titania, and Oberon were taken from Jacobson, 1992.[26] Masses of all other moons were calculated assuming a density of 1.3 g/cm3 and using given radii.
  7. ↑ Negative orbital periods indicate a retrograde orbit around Uranus (opposite to the planet's rotation).
  8. ↑ Inclination measures the angle between the moon's orbital plane and the plane defined by Uranus's equator.
  9. ↑ 9.0 9.1 Detected in 2001, published in 2003.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "Planet and Satellite Names and Discoverers". Gazetteer of Planetary Nomenclature. USGS Astrogeology. July 21, 2006. https://planetarynames.wr.usgs.gov/Page/Planets. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 Smith, B. A.; Soderblom, L. A.; Beebe, A.; Bliss, D.; Boyce, J. M.; Brahic, A.; Briggs, G. A.; Brown, R. H. et al. (4 July 1986). "Voyager 2 in the Uranian System: Imaging Science Results". Science 233 (4759): 43–64. doi:10.1126/science.233.4759.43. PMID 17812889. Bibcode: 1986Sci...233...43S. https://zenodo.org/record/1230972. 
  3. ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 3.10 3.11 3.12 Sheppard, S. S.; Jewitt, D.; Kleyna, J. (2005). "An Ultradeep Survey for Irregular Satellites of Uranus: Limits to Completeness". The Astronomical Journal 129 (1): 518–525. doi:10.1086/426329. Bibcode: 2005AJ....129..518S. 
  4. ↑ Herschel, John (1834). "On the Satellites of Uranus". Monthly Notices of the Royal Astronomical Society 3 (5): 35–36. doi:10.1093/mnras/3.5.35. Bibcode: 1834MNRAS...3...35H. 
  5. ↑ Lassell, W. (1851). "On the interior satellites of Uranus". Monthly Notices of the Royal Astronomical Society 12: 15–17. doi:10.1093/mnras/12.1.15. Bibcode: 1851MNRAS..12...15L. 
  6. ↑ Lassell, W. (1848). "Observations of Satellites of Uranus". Monthly Notices of the Royal Astronomical Society 8 (3): 43–44. doi:10.1093/mnras/8.3.43. Bibcode: 1848MNRAS...8...43L. 
  7. ↑ Lassell, William (December 1851). "Letter from William Lassell, Esq., to the Editor". Astronomical Journal 2 (33): 70. doi:10.1086/100198. Bibcode: 1851AJ......2...70L. 
  8. ↑ 8.0 8.1 8.2 Kuiper, G. P. (1949). "The Fifth Satellite of Uranus". Publications of the Astronomical Society of the Pacific 61 (360): 129. doi:10.1086/126146. Bibcode: 1949PASP...61..129K. 
  9. ↑ Kaempffert, Waldemar (December 26, 1948). "Science in Review: Research Work in Astronomy and Cancer Lead Year's List of Scientific Developments". The New York Times: p. 87. ISSN 0362-4331. https://query.nytimes.com/gst/abstract.html?res=9F05EFDF143AE33BBC4E51DFB4678383659EDE&legacy=true. 
  10. ↑ Karkoschka, Erich (May 18, 1999). "S/1986 U 10". IAU Circular 7171: 1. ISSN 0081-0304. Bibcode: 1999IAUC.7171....1K. http://www.cbat.eps.harvard.edu/iauc/07100/07171.html. Retrieved 2011-11-02. 
  11. ↑ 11.0 11.1 Karkoschka, Erich (2001). "Voyager's Eleventh Discovery of a Satellite of Uranus and Photometry and the First Size Measurements of Nine Satellites". Icarus 151 (1): 69–77. doi:10.1006/icar.2001.6597. Bibcode: 2001Icar..151...69K. 
  12. ↑ 12.0 12.1 12.2 12.3 12.4 Showalter, Mark R.; Lissauer, Jack J. (2006-02-17). "The Second Ring-Moon System of Uranus: Discovery and Dynamics". Science 311 (5763): 973–977. doi:10.1126/science.1122882. PMID 16373533. Bibcode: 2006Sci...311..973S. 
  13. ↑ Sheppard, Scott S.; Jewitt, D. C. (2003-10-09). "S/2003 U 3". IAU Circular 8217: 1. ISSN 0081-0304. Bibcode: 2003IAUC.8217....1S. http://www.cbat.eps.harvard.edu/iauc/08200/08217.html. Retrieved 2011-11-02. 
  14. ↑ Hughes, D. W. (1994). "The Historical Unravelling of the Diameters of the First Four Asteroids". R.A.S. Quarterly Journal 35 (3): 334–344. Bibcode: 1994QJRAS..35..331H. 
  15. ↑ Denning, W.F. (October 22, 1881). "The centenary of the discovery of Uranus". Scientific American Supplement (303). http://www.infomotions.com/etexts/gutenberg/dirs/etext05/7030310.htm. 
  16. ↑ William Lassell (1852). "Beobachtungen der Uranus-Satelliten". Astronomische Nachrichten 34: 325. Bibcode: 1852AN.....34..325.. 
  17. ↑ Tyler, G.L.; Sweetnam, D.L. et al. (1989). "Voyager radio science observations of Neptune and Triton". Science 246 (4936): 1466–73. doi:10.1126/science.246.4936.1466. PMID 17756001. Bibcode: 1989Sci...246.1466T. 
  18. ↑ 18.0 18.1 18.2 Thomas, P. C. (1988). "Radii, shapes, and topography of the satellites of Uranus from limb coordinates". Icarus 73 (3): 427–441. doi:10.1016/0019-1035(88)90054-1. Bibcode: 1988Icar...73..427T. 
  19. ↑ Esposito, L. W. (2002). "Planetary rings". Reports on Progress in Physics 65 (12): 1741–1783. doi:10.1088/0034-4885/65/12/201. Bibcode: 2002RPPh...65.1741E. 
  20. ↑ Chancia, R.O.; Hedman, M.M. (2016). "Are there moonlets near Uranus' alpha and beta rings?". The Astronomical Journal 152 (6): 211. doi:10.3847/0004-6256/152/6/211. Bibcode: 2016AJ....152..211C. 
  21. ↑ 21.0 21.1 Karkoschka, Erich (2001). "Comprehensive Photometry of the Rings and 16 Satellites of Uranus with the Hubble Space Telescope". Icarus 151 (1): 51–68. doi:10.1006/icar.2001.6596. Bibcode: 2001Icar..151...51K. 
  22. ↑ Dumas, Christophe; Smith, Bradford A.; Terrile, Richard J. (2003). "Hubble Space Telescope NICMOS Multiband Photometry of Proteus and Puck". The Astronomical Journal 126 (2): 1080–1085. doi:10.1086/375909. Bibcode: 2003AJ....126.1080D. 
  23. ↑ Duncan, Martin J.; Lissauer, Jack J. (1997). "Orbital Stability of the Uranian Satellite System". Icarus 125 (1): 1–12. doi:10.1006/icar.1996.5568. Bibcode: 1997Icar..125....1D. 
  24. ↑ "Uranus's colliding moons". astronomy.com. 2017. http://www.astronomy.com/news/2017/09/uranus-colliding-moons. 
  25. ↑ 25.0 25.1 French, Robert S.; Showalter, Mark R. (August 2012). "Cupid is doomed: An analysis of the stability of the inner uranian satellites". Icarus 220 (2): 911–921. doi:10.1016/j.icarus.2012.06.031. Bibcode: 2012Icar..220..911F. 
  26. ↑ 26.0 26.1 Jacobson, R. A.; Campbell, J. K.; Taylor, A. H.; Synnott, S. P. (June 1992). "The masses of Uranus and its major satellites from Voyager tracking data and earth-based Uranian satellite data". The Astronomical Journal 103 (6): 2068–2078. doi:10.1086/116211. Bibcode: 1992AJ....103.2068J. 
  27. ↑ Mousis, O. (2004). "Modeling the thermodynamical conditions in the Uranian subnebula – Implications for regular satellite composition". Astronomy & Astrophysics 413: 373–380. doi:10.1051/0004-6361:20031515. Bibcode: 2004A&A...413..373M. 
  28. ↑ Hunt, Garry E.; Patrick Moore (1989). Atlas of Uranus. Cambridge University Press. pp. 78–85. ISBN 0-521-34323-2. https://archive.org/details/atlasofuranus00hunt_1/page/78. 
  29. ↑ Detre, Ö. H.; Müller, T. G.; Klaas, U.; Marton, G.; Linz, H.; Balog, Z. (2020). "Herschel -PACS photometry of the five major moons of Uranus". Astronomy & Astrophysics 641: A76. doi:10.1051/0004-6361/202037625. ISSN 0004-6361. Bibcode: 2020A&A...641A..76D. 
  30. ↑ Farkas-Takács, A.; Kiss, Cs.; Pál, A.; Molnár, L.; Szabó, Gy. M.; Hanyecz, O.; Sárneczky, K.; Szabó, R. et al. (2017-08-31). "Properties of the Irregular Satellite System around Uranus Inferred from K2 , Herschel , and Spitzer Observations". The Astronomical Journal 154 (3): 119. doi:10.3847/1538-3881/aa8365. ISSN 1538-3881. Bibcode: 2017AJ....154..119F. 
  31. ↑ 31.0 31.1 31.2 Hussmann, Hauke; Sohl, Frank; Spohn, Tilman (November 2006). "Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects". Icarus 185 (1): 258–273. doi:10.1016/j.icarus.2006.06.005. Bibcode: 2006Icar..185..258H. 
  32. ↑ Grundy, W. M.; Young, L. A.; Spencer, J. R.; Johnson, R. E.; Young, E. F.; Buie, M. W. (October 2006). "Distributions of H2O and CO2 ices on Ariel, Umbriel, Titania, and Oberon from IRTF/SpeX observations". Icarus 184 (2): 543–555. doi:10.1016/j.icarus.2006.04.016. Bibcode: 2006Icar..184..543G. 
  33. ↑ Pappalardo, R. T.; Reynolds, S. J.; Greeley, R. (1996). "Extensional tilt blocks on Miranda: Evidence for an upwelling origin of Arden Corona". Journal of Geophysical Research 102 (E6): 13,369–13,380. doi:10.1029/97JE00802. Bibcode: 1997JGR...10213369P. https://www.agu.org/pubs/crossref/1997/97JE00802.shtml. 
  34. ↑ Tittemore, William C.; Wisdom, Jack (June 1990). "Tidal evolution of the Uranian satellites: III. Evolution through the Miranda-Umbriel 3:1, Miranda-Ariel 5:3, and Ariel-Umbriel 2:1 mean-motion commensurabilities". Icarus 85 (2): 394–443. doi:10.1016/0019-1035(90)90125-S. Bibcode: 1990Icar...85..394T. 
  35. ↑ Tittemore, W. C. (September 1990). "Tidal heating of Ariel". Icarus 87 (1): 110–139. doi:10.1016/0019-1035(90)90024-4. Bibcode: 1990Icar...87..110T. 
  36. ↑ Tittemore, W. C.; Wisdom, J. (1989). "Tidal Evolution of the Uranian Satellites II. An Explanation of the Anomalously High Orbital Inclination of Miranda". Icarus 78 (1): 63–89. doi:10.1016/0019-1035(89)90070-5. Bibcode: 1989Icar...78...63T. http://groups.csail.mit.edu/mac/users/wisdom/TittemoreWisdomII.pdf. 
  37. ↑ Malhotra, R.; Dermott, S. F. (1990). "The Role of Secondary Resonances in the Orbital History of Miranda". Icarus 85 (2): 444–480. doi:10.1016/0019-1035(90)90126-T. Bibcode: 1990Icar...85..444M. 
  38. ↑ 38.0 38.1 Widemann, T.; Sicardy, B.; Dusser, R.; Martinez, C.; Beisker, W.; Bredner, E.; Dunham, D.; Maley, P. et al. (February 2009). "Titania's radius and an upper limit on its atmosphere from the September 8, 2001 stellar occultation". Icarus 199 (2): 458–476. doi:10.1016/j.icarus.2008.09.011. Bibcode: 2009Icar..199..458W. http://www.lesia.obspm.fr/perso/thomas-widemann/eprint/Widemann_etal2009.pdf. Retrieved September 4, 2015. 
  39. ↑ 39.0 39.1 "Natural Satellites Ephemeris Service". IAU: Minor Planet Center. http://www.minorplanetcenter.org/iau/NatSats/NaturalSatellites.html. 
  40. ↑ Brozović, Marina; Jacobson, Robert A. (April 2009). "The Orbits of the Outer Uranian Satellites". The Astronomical Journal 137 (4): 3834–3842. doi:10.1088/0004-6256/137/4/3834. Bibcode: 2009AJ....137.3834B. 
  41. ↑ 41.0 41.1 41.2 41.3 41.4 Williams, Dr. David R. (2007-11-23). "Uranian Satellite Fact Sheet". NASA (National Space Science Data Center). http://nssdc.gsfc.nasa.gov/planetary/factsheet/uraniansatfact.html. 
  42. ↑ Farkas-Takács, A.Expression error: Unrecognized word "etal". (September 2017). "Properties of the Irregular Satellite System around Uranus Inferred from K2, Herschel, and Spitzer Observations". The Astronomical Journal 154 (3): 13. doi:10.3847/1538-3881/aa8365. 119. Bibcode: 2017AJ....154..119F. 
  43. ↑ Jacobson, R. A. (1998). "The Orbits of the Inner Uranian Satellites From Hubble Space Telescope and Voyager 2 Observations". The Astronomical Journal 115 (3): 1195–1199. doi:10.1086/300263. Bibcode: 1998AJ....115.1195J. 

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