Moons of Uranus

Uranus, the 7th planet from the sun has a total of 27 natural satellites. This is a complete list of natural satellites.
As with all lists, it will always remain incomplete. Please take some time to help complete the list. We will really appreciate your contribution!
Moons of Mars
Moons of Jupiter
Moons of Saturn
Moons of Uranus
Moons of Neptune
Moons of Pluto
Moons of Haumea
==Groups==
===Inner Moons===
As of 2020, Uranus has 13 inner moons. All of their orbits lie inside Miranda's orbit. 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. 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. 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.
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%. They are composed of water ice contaminated with a dark material, probably radiation-processed organics.
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. Desdemona may collide with Cressida within the next million years, and Cupid will likely collide with Belinda in the next 10 million years; Perdita and Juliet may be involved in later collisions. Because of this, the rings and inner moons may be under constant flux, with moons colliding and re-accreting on short timescales.
===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. All these moons are relatively dark objects: their geometrical albedo varies between 30 and 50%, whereas their Bond albedo is between 10 and 23%. 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. 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. This view is supported by their large thermal inertia, a surface property they share with dwarf planets like Pluto and Haumea. It differs strongly from the thermal behaviour of the Uranian irregular moons that is comparable to classical trans-Neptunian objects. This suggests a separate origin.
All major moons comprise approximately equal amounts rock and ice, except Miranda, which is made primarily of ice. The ice component may include ammonia and carbon dioxide. 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. Extensional processes associated with upwelling diapirs are likely responsible for the origin of the coronae. Ariel appears to have the youngest surface with the fewest impact craters, while Umbriel's appears oldest. 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. 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. The largest Uranian moons may be internally differentiated, with rocky cores at their centers surrounded by ice mantles. Titania and Oberon may harbor liquid water oceans at the core/mantle boundary. 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.
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). 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, 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 hemispheric 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===
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. 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.
Uranus's irregular moons range in size from 120–200 km (Sycorax) to about 20 km (Trinculo). 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. The outer group (a > 0.15 rH) includes satellites with high eccentricity (~0.5): Sycorax, Prospero, Setebos, and Ferdinand.
The intermediate inclinations 60° < i < 140° are devoid of known moons due to the Kozai instability. In this instability region, solar perturbations at apoapsis 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.
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.
==List==
Key
Inner Moons	Major Moons	Irregular Moons
(retrograde)	Irregular Moons
(prograde)
i 	† 	‡	±
Numeral	Name 	Diameter 	Gravity 	Escape Velocity	Orbital Period	Group Label	Year of Discovery
- 	Uranus 	50724 km 	8.69 m/s² 	21.3 km/s 	84 earth years	- 	1781
I 	Ariel 	1157.8±1.2 km 	0.249 m/s² 	0.537 km/s 	2.52038 days 	† 	1851
II 	Umbriel 	1169.4±5.6 km 	0.25 m/s² 	0.54 km/s 	4.14418 days 	† 	1851
III 	Titania 	1576.8±1.2 km 	0.365 m/s² 	0.759 km/s 	8.70587 days 	† 	1781
IV 	Oberon 	1522.8±5.2 km 	0.354 m/s² 	0.734 km/s 	3.4632 days 	† 	1781
V 	Miranda 	471.6 ± 1.4 km	0.077 m/s² 	0.19 km/s 	1.41348 days 	† 	1948
VI 	Cordelia 	40 ± 6 km 	~0.0073 m/s²	0.017 km/s 	0.33503 days 	i 	1986
VII 	Ophelia 	43 ± 8 km 	~0.007 m/s² 	0.018 km/s 	0.37640 days 	i 	1986
VIII 	Bianca 	51 ± 4 km 	~0.0086 m/s²	0.022 km/s 	0.46357 days 	i 	1986
IX 	Cressida 	80 ± 4 km 	~0.013 m/s² 	0.034 km/s 	0.46357 days 	i 	1986
X 	Desdemona	64 ± 8 km 	~0.011 m/s² 	0.027 km/s 	0.47365 days 	i 	1986
XI 	Juliet 	94 ± 8 km 	~0.016 m/s² 	0.04 km/s 	0.49307 days 	i 	1986
XII 	Portia 	135 ± 8 km 	~0.023 m/s² 	0.058 km/s 	0.51320 days 	i 	1986
XII 	Rosalind 	72 ± 12 km 	~0.012 m/s² 	0.031 km/s 	0.55846 days 	i 	1986
XIV 	Belinda 	90 ± 16 km 	~0.014 m/s² 	~0.034 km/s 	0.62353 days 	i 	1986
XV 	Puck 	162 ± 4 km 	0.028 m/s² 	0.069 km/s 	0.76183 days 	i 	1985
XVI 	Caliban 	~42 km 	? 	? 	579.73 days 	‡ 	1997
XVII 	Sycorax 	~157 km 	? 	? 	1288.38 days 	‡ 	1997
XVIII 	Prospero 	~50 km 	~0.0063 m/s²	~0.021 km/s 	1978.37 days 	‡ 	1999
XIX 	Setebos 	~48 km 	~0.0063 m/s²	~0.0204 km/s 	2225.08 days 	‡ 	1999
XX 	Stephano 	~32 km 	~0.0041 m/s²	~0.013 km/s 	677.47 days 	‡ 	1999
XXI 	Trinculo 	~18 km 	~0.0021 m/s²	0.007 km/s 	749.4 days 	‡ 	2001
XXII 	Francisco	~22 km 	~0.0025 m/s²	0.0094 km/s 	267.09 days 	‡ 	2003
XXIII 	Margaret 	~20 km 	~0.0023 m/s²	~0.0085 km/s 	1661 days 	± 	2003
XXIV 	Ferdinand	~12 km 	? 	? 	2790.03 days 	‡ 	2003
XXV 	Perdita 	30 ± 6 km 	~0.0047 m/s²	~0.0011 km/s 	0.638 days 	i 	1999
XXVI 	Mab 	~18 km 	~0.0044 m/s²	~0.011 km/s 	0.923 days 	i 	2003
XXVII 	Cupid 	~18 km 	~0.0031 m/s²	~0.0076 km/s 	0.618 days 	i 	2003
==Gallery==
File:Titania.jpg|Titania
File:Stephano.jpg|Stephano
File:Setebos.jpg|Setebos
File:Umbriel.jpg|Umbriel
File:Sycorax.gif|Sycorax
File:Prospero.jpg|Prospero
File:Ophelia.png|Ophelia
File:Oberon.jpg|Oberon
File:Mabmoon.png|Mab
File:Juliet.png|Juliet
File:Margaret.gif|Margaret
File:Portia.jpg|Portia
File:Perdita.png|Perdita
File:Miranda.jpg|Miranda
File:Puck.png|Puck
File:Cordeliamoon.png|Cordelia
File:Cressida.png|Cressida
File:Bianca.png|Bianca
File:Cupid.png|Cupid
File:Belinda.gif|Belinda
File:Caliban.jpg|Caliban
File:Desdemona.png|Desdemona
File:Ferdinand.jpg|Ferdinand
File:Ariel.jpg|Ariel
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