Moons of Uranus

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

Uranus is the seventh planet of the Solar System; it has 27 known moons, all of which are named after characters from the works of William Shakespeare and Alexander Pope.[1] Uranus's moons are divided into three groups: thirteen inner moons, five major moons, and nine irregular moons. The inner moons are small dark bodies that share common properties and origins with Uranus's rings. The five major moons are massive enough to have reached hydrostatic 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, and about one-twentieth the mass of the 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, and 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 have planetary mass, 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 retroactively 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 2016, 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

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 sylphs Ariel and 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). At first, the outermost moons were all named after characters from one play, The Tempest; but with Margaret being named from Much Ado About Nothing that trend has ended.[8]

The relative masses of the Uranian moons. The five rounded moons vary from Miranda at 0.7% to Titania at almost 40% of the total mass. The other moons collectively constitute 0.1%, and are barely visible at this scale.

Some asteroids share names with moons of Uranus: 171 Ophelia, 218 Bianca, 593 Titania, 666 Desdemona, 763 Cupido, and 2758 Cordelia.

Characteristics and groups

Schematic of the Uranian moon–ring system

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

As of 2016, Uranus is known to have 13 inner moons.[12] Their orbits lie inside that of Miranda. All inner moons are intimately connected to 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 as 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' 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. 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 either Cressida or Juliet within the next 100 million years.[23]

The five largest moons of Uranus compared at their proper relative sizes and brightnesses. From left to right (in order of increasing distance from Uranus): Miranda, Ariel, Umbriel, Titania, and Oberon.

Large moons

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.[24] 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.[25][26]

Artist's conception of the Sun's path in the summer sky of a major moon of Uranus (which shares Uranus's axial tilt)

All major moons comprise approximately equal amounts rock and ice, except Miranda, which is made primarily of ice.[27] The ice component may include ammonia and carbon dioxide.[28] 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.[29] 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.[30][31] 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.[32][33] The largest Uranian moons may be internally differentiated, with rocky cores at their centers surrounded by ice mantles.[27] Titania and Oberon may harbor liquid water oceans at the core/mantle boundary.[27] 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.[34]

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] 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.

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.

Irregular moons

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.[35]

List

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. 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.

Uranian moons
Order
[lower-alpha 4]		 Label
[lower-alpha 5]		 Name Pronunciation
(key)		 Image Diameter
(km)[lower-alpha 6]		 Mass
(×1018 kg)[lower-alpha 7]		 Semi-major axis
(km)[37]		 Orbital period
(d)[37][lower-alpha 8]		 Inclination
(°)[37][lower-alpha 9]		 Eccentricity
[38]		 Discovery
year[1]		 Discoverer
[1]
1 VI Cordelia Cordelia /kɔːrˈdiːliə/ 40 ± 6
(50 × 36) 		0.044 49770 0.335034 0.08479° 0.00026 1986 Terrile
(Voyager 2)
2 VII Ophelia Ophelia /oʊˈfiːliə/ 43 ± 8
(54 × 38) 		0.053 53790 0.376400 0.1036° 0.00992 1986 Terrile
(Voyager 2)
3 VIII Bianca /biˈɑːŋkə/ 51 ± 4
(64 × 46) 		0.092 59170 0.434579 0.193° 0.00092 1986 Smith
(Voyager 2)
4 IX Cressida Cressida /ˈkrɛsᵻdə/ 80 ± 4
(92 × 74) 		0.34 61780 0.463570 0.006° 0.00036 1986 Synnott
(Voyager 2)
5 X Desdemona Desdemona /ˌdɛzdᵻˈmoʊnə/ 64 ± 8
(90 × 54) 		0.18 62680 0.473650 0.11125° 0.00013 1986 Synnott
(Voyager 2)
6 XI Juliet Juliet /ˈdʒuːliət/ 94 ± 8
(150 × 74) 		0.56 64350 0.493065 0.065° 0.00066 1986 Synnott
(Voyager 2)
7 XII Portia Portia /ˈpɔːrʃə/ 135 ± 8
(156 × 126) 		1.70 66090 0.513196 0.059° 0.00005 1986 Synnott
(Voyager 2)
8 XIII Rosalind Rosalind /ˈrɒzəlᵻnd/ 72 ± 12 0.25 69940 0.558460 0.279° 0.00011 1986 Synnott
(Voyager 2)
9 XXVII Cupid Cupid /ˈkjuːpᵻd/ ≈ 18 0.0038 74800 0.618 0.1° 0.0013 2003 Showalter and
Lissauer
10 XIV Belinda Belinda /bᵻˈlɪndə/
90 ± 16
(128 × 64) 		0.49 75260 0.623527 0.031° 0.00007 1986 Synnott
(Voyager 2)
11 XXV Perdita Perdita /pərˈdiːtə/ 30 ± 6 0.018 76400 0.638 0.0° 0.0012 1999 Karkoschka
(Voyager 2)
12 XV Puck Puck /ˈpʌk/
162 ± 4 2.90 86010 0.761833 0.3192° 0.00012 1985 Synnott
(Voyager 2)
13 XXVI Mab Mab /ˈmæb/
≈ 25 0.01 97700 0.923 0.1335° 0.0025 2003 Showalter and
Lissauer
14 V Miranda †Miranda /mᵻˈrændə/
471.6 ± 1.4
(481 × 468 × 466) 		65.9±7.5 129390 1.413479 4.232° 0.0013 1948 Kuiper
15 I Ariel †Ariel /ˈɛəriəl/
1157.8±1.2
(1162 × 1156 × 1155) 		1353±120 191020 2.520379 0.260° 0.0012 1851 Lassell
16 II Umbriel †Umbriel /ˈʌmbriəl/
1169.4±5.6 1172±135 266300 4.144177 0.205° 0.0039 1851 Lassell
17 III Titania †Titania /tᵻˈteɪnjə/
1576.8±1.2 3527±90 435910 8.705872 0.340° 0.0011 1787 Herschel
18 IV Oberon †Oberon /ˈoʊbərɒn/
1522.8±5.2 3014±75 583520 13.463239 0.058° 0.0014 1787 Herschel
19 XXII Francisco ‡Francisco /frænˈsɪskoʊ/ ≈ 22 0.0072 4276000 −266.56 147.459° 0.1459 2003[lower-alpha 10] Holman et al.
20 XVI Caliban ‡Caliban /ˈkælᵻbæn/ ≈ 72 0.25 7230000 −579.50 139.885° 0.1587 1997 Gladman et al.
21 XX Stephano ‡Stephano /ˈstɛfənoʊ/ ≈ 32 0.022 8002000 −676.50 141.873° 0.2292 1999 Gladman et al.
22 XXI Trinculo ‡Trinculo /ˈtrɪŋkjᵿloʊ/ ≈ 18 0.0039 8571000 −758.10 166.252° 0.2200 2001 Holman et al.
23 XVII Sycorax‡Sycorax /ˈsɪkəræks/ 165+36
−42 		2.30 12179000 −1283.4 152.456° 0.5224 1997 Nicholson et al.
24 XXIII °Margaret Margaret /ˈmɑːrɡərᵻt/ ≈ 20 0.0054 14345000 1694.8 51.455° 0.6608 2003 Sheppard and
Jewitt
25 XVIII Prospero ‡Prospero /ˈprɒspəroʊ/ ≈ 50 0.085 16418000 −1992.8 146.017° 0.4448 1999 Holman et al.
26 XIX Setebos ‡Setebos /ˈsɛtᵻbʌs/ ≈ 48 0.075 17459000 −2202.3 145.883° 0.5914 1999 Kavelaars et al.
27 XXIV Ferdinand ‡Ferdinand /ˈfɜːrdᵻnænd/ ≈ 20 0.0054 20900000 −2823.4 167.346° 0.3682 2003[lower-alpha 10] Holman et al.

Sources: NASA/NSSDC,[37] 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 Natural Satellites Ephemeris Service.[35] The irregulars are significantly perturbed by the Sun.[3]

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. ↑ Order refers to the position among other moons with respect to their average distance from Uranus.
  5. ↑ Label refers to the Roman numeral attributed to each moon in order of their discovery.[1]
  6. ↑ 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.[34] 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 were taken from Sheppard, 2005.[3] The diameter of Sycorax is from Lellouch, 2013.[36]
  7. ↑ Masses of Miranda, Ariel, Umbriel, Titania, and Oberon were taken from Jacobson, 1992.[24] Masses of all other moons were calculated assuming a density of 1.3 g/cm3 and using given radii.
  8. ↑ Negative orbital periods indicate a retrograde orbit around Uranus (opposite to the planet's rotation).
  9. ↑ Inclination measures the angle between the moon's orbital plane and the plane defined by Uranus's equator.
  10. 1 2 Detected in 2001, published in 2003.

References

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  2. 1 2 3 4 5 6 7 Smith, B. A.; Soderblom, L. A.; Beebe, A.; Bliss, D.; Boyce, J. M.; Brahic, A.; Briggs, G. A.; Brown, R. H.; Collins, S. A. (4 July 1986). "Voyager 2 in the Uranian System: Imaging Science Results". Science. 233 (4759): 43–64. Bibcode:1986Sci...233...43S. PMID 17812889. doi:10.1126/science.233.4759.43.
  3. 1 2 3 4 5 6 7 8 9 10 11 12 13 Sheppard, S. S.; Jewitt, D.; Kleyna, J. (2005). "An Ultradeep Survey for Irregular Satellites of Uranus: Limits to Completeness". The Astronomical Journal. 129: 518–525. Bibcode:2005AJ....129..518S. arXiv:astro-ph/0410059 Freely accessible. doi:10.1086/426329.
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  5. ↑ Lassell, W. (1851). "On the interior satellites of Uranus". Monthly Notices of the Royal Astronomical Society. 12: 15–17. Bibcode:1851MNRAS..12...15L. doi:10.1093/mnras/12.1.15.
  6. ↑ Lassell, W. (1848). "Observations of Satellites of Uranus". Monthly Notices of the Royal Astronomical Society. 8 (3): 43–44. Bibcode:1848MNRAS...8...43.. doi:10.1093/mnras/8.3.43.
  7. ↑ Lassell, William (December 1851). "Letter from William Lassell, Esq., to the Editor". Astronomical Journal. 2 (33): 70. Bibcode:1851AJ......2...70L. doi:10.1086/100198.
  8. 1 2 3 Kuiper, G. P. (1949). "The Fifth Satellite of Uranus". Publications of the Astronomical Society of the Pacific. 61 (360): 129. Bibcode:1949PASP...61..129K. doi:10.1086/126146.
  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 (Late City ed.). p. 87. ISSN 0362-4331.
  10. ↑ Karkoschka, Erich (May 18, 1999). "S/1986 U 10". IAU Circular. 7171. ISSN 0081-0304. Retrieved 2011-11-02.
  11. 1 2 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. Bibcode:2001Icar..151...69K. doi:10.1006/icar.2001.6597.
  12. 1 2 3 4 5 Showalter, Mark R.; Lissauer, Jack J. (2006-02-17). "The Second Ring-Moon System of Uranus: Discovery and Dynamics". Science. 311 (5763): 973–977. Bibcode:2006Sci...311..973S. PMID 16373533. doi:10.1126/science.1122882.
  13. ↑ Sheppard, Scott S.; Jewitt, D. C. (2003-10-09). "S/2003 U 3". IAU Circular. 8217. ISSN 0081-0304. 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.
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  16. ↑ William Lassell (1852). "Beobachtungen der Uranus-Satelliten". Astronomische Nachrichten. 34: 325. Bibcode:1852AN.....34..325. Retrieved 2008-12-18.
  17. ↑ Tyler, G.L.; Sweetnam, D.L.; et al. (1989). "Voyager radio science observations of Neptune and Triton". Science. 246 (4936): 1466–73. Bibcode:1989Sci...246.1466T. PMID 17756001. doi:10.1126/science.246.4936.1466.
  18. 1 2 3 Thomas, P. C. (1988). "Radii, shapes, and topography of the satellites of Uranus from limb coordinates". Icarus. 73 (3): 427–441. Bibcode:1988Icar...73..427T. doi:10.1016/0019-1035(88)90054-1.
  19. ↑ Esposito, L. W. (2002). "Planetary rings". Reports On Progress In Physics. 65 (12): 1741–1783. Bibcode:2002RPPh...65.1741E. doi:10.1088/0034-4885/65/12/201.
  20. ↑ Chancia, R.O.; Hedman, M.M. (2016). "Are there moonlets near Uranus' alpha and beta rings?". The Astronomical Journal. arXiv:1610.02376 Freely accessible. doi:10.3847/0004-6256/152/6/211.
  21. 1 2 Karkoschka, Erich (2001). "Comprehensive Photometry of the Rings and 16 Satellites of Uranus with the Hubble Space Telescope". Icarus. 151 (1): 51–68. Bibcode:2001Icar..151...51K. doi:10.1006/icar.2001.6596.
  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. Bibcode:2003AJ....126.1080D. doi:10.1086/375909.
  23. ↑ Duncan, Martin J.; Lissauer, Jack J. (1997). "Orbital Stability of the Uranian Satellite System". Icarus. 125 (1): 1–12. Bibcode:1997Icar..125....1D. doi:10.1006/icar.1996.5568.
  24. 1 2 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. Bibcode:1992AJ....103.2068J. doi:10.1086/116211.
  25. ↑ Mousis, O. (2004). "Modeling the thermodynamical conditions in the Uranian subnebula – Implications for regular satellite composition". Astronomy & Astrophysics. 413: 373–380. Bibcode:2004A&A...413..373M. doi:10.1051/0004-6361:20031515.
  26. ↑ Hunt, Garry E.; Patrick Moore (1989). Atlas of Uranus. Cambridge University Press. pp. 78–85. ISBN 0-521-34323-2.
  27. 1 2 3 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. Bibcode:2006Icar..185..258H. doi:10.1016/j.icarus.2006.06.005.
  28. ↑ 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. Bibcode:2006Icar..184..543G. arXiv:0704.1525 Freely accessible. doi:10.1016/j.icarus.2006.04.016.
  29. ↑ 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. Bibcode:1997JGR...10213369P. doi:10.1029/97JE00802.
  30. ↑ 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. Bibcode:1990Icar...85..394T. doi:10.1016/0019-1035(90)90125-S.
  31. ↑ Tittemore, W. C. (September 1990). "Tidal heating of Ariel". Icarus. 87 (1): 110–139. Bibcode:1990Icar...87..110T. doi:10.1016/0019-1035(90)90024-4.
  32. ↑ Tittemore, W. C.; Wisdom, J. (1989). "Tidal Evolution of the Uranian Satellites II. An Explanation of the Anomalously High Orbital Inclination of Miranda" (PDF). Icarus. 78 (1): 63–89. Bibcode:1989Icar...78...63T. doi:10.1016/0019-1035(89)90070-5.
  33. ↑ Malhotra, R.; Dermott, S. F. (1990). "The Role of Secondary Resonances in the Orbital History of Miranda". Icarus. 85 (2): 444–480. Bibcode:1990Icar...85..444M. doi:10.1016/0019-1035(90)90126-T.
  34. 1 2 Widemann, T.; Sicardy, B.; Dusser, R.; Martinez, C.; Beisker, W.; Bredner, E.; Dunham, D.; Maley, P.; Lellouch, E.; Arlot, J. -E.; Berthier, J.; Colas, F.; Hubbard, W. B.; Hill, R.; Lecacheux, J.; Lecampion, J. -F.; Pau, S.; Rapaport, M.; Roques, F.; Thuillot, W.; Hills, C. R.; Elliott, A. J.; Miles, R.; Platt, T.; Cremaschini, C.; Dubreuil, P.; Cavadore, C.; Demeautis, C.; Henriquet, P.; Labrevoir, O. (February 2009). "Titania's radius and an upper limit on its atmosphere from the September 8, 2001 stellar occultation" (PDF). Icarus. 199 (2): 458–476. Bibcode:2009Icar..199..458W. doi:10.1016/j.icarus.2008.09.011.
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  38. ↑ 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. Bibcode:1998AJ....115.1195J. doi:10.1086/300263.
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