Moons of Uranus

Short description: Natural satellites of the planet Uranus

A near-infrared image of the six largest moons and eight largest inner moons of Uranus as captured by the James Webb Space Telescope on 4 September 2023

There are 29 known moons of the planet Uranus.[1] The 27 with names are named after characters that appear in, or are mentioned in William Shakespeare's plays and Alexander Pope's poem The Rape of the Lock.[2] Uranus's moons are divided into three groups: fourteen inner moons, five major moons, and ten irregular moons. The inner and major moons all have prograde orbits and are cumulatively classified as regular moons. In contrast, the orbits of the irregular moons are distant, highly inclined, and 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.[3] 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.[4]

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).[2] These five may be in hydrostatic equilibrium. The remaining moons were discovered after 1985, either during the Voyager 2 flyby mission or with the aid of advanced Earth-based telescopes.[3][4]

## Contents

* 1 Discovery
* 1.1 Spurious moons
* 2 Names
* 3 Characteristics and groups
* 3.1 Inner moons
* 3.2 Large moons
* 3.3 Irregular moons
* 4 List of moons
* 5 See also
* 6 Notes
* 7 References
* 8 External links

## 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.[5] 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.[6] 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).[7] With the confirmation of Ariel and Umbriel, Lassell numbered the moons I through IV from Uranus outward, and this finally stuck.[8] In 1852, Herschel's son John Herschel gave the four then-known moons their names.[9]

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.[9][10] Decades later, the flyby of the Voyager 2 space probe in January 1986 led to the discovery of ten further inner moons.[3] Another satellite, Perdita, was discovered in 1999[11] by Erich Karkoschka after studying old Voyager photographs.[12]

Uranus was the last giant planet without any known irregular moons until 1997, when astronomers using ground-based telescopes discovered Sycorax and Caliban. From 1999 to 2003, astronomers continued searching for irregular moons of Uranus using more powerful ground-based telescopes, resulting in the discovery of seven more Uranian irregular moons.[4] In addition, two small inner moons, Cupid and Mab, were discovered using the Hubble Space Telescope in 2003.[13] No other discoveries were reported until 2024, when Scott Sheppard and colleagues announced the discovery of one irregular moon of Uranus (S/2023 U 1) from 2023 observations by the Subaru Telescope at Mauna Kea, Hawaii.[14][15]

In August 2025, a team of astronomers led by Maryame El Moutamid at the Southwest Research Institute announced the discovery of a new inner moon of Uranus (Uranus XXVIII) in James Webb Space Telescope images from February 2025. It was not detected earlier by Voyager 2 and the Hubble Space Telescope because it was too small and faint.[1][16]

### Spurious moons

After Herschel discovered Titania and Oberon on 11 January 1787, he subsequently believed that he had observed four other moons: two on 18 January and 9 February 1790, and two more on 28 February and 26 March 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 besides 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).[17] 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.[18]

## Names

Main article: Astronomy:Naming of moons

See also: Astronomy:Name conflicts with minor planets

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 spirit in Shakespeare's The Tempest).[19] It is uncertain if John Herschel was the originator of the names, or if it was instead William Lassell (who discovered Ariel and Umbriel) who chose the names and asked Herschel for permission.[20]

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 human character in Shakespeare's The Tempest.[9] 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.[20]

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

Pie chart showing the relative masses of the 5 major (rounded) Uranian moons

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,[22] 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

See also: Astronomy:Inner moon and Rings of Uranus

Schematic of the Uranian moon–ring system, excluding Uranus XXVIII, which was not known at the time of drawing

As of 2026, Uranus is known to have 14 inner moons, whose orbits all lie inside that of Miranda.[13] Some of the inner moons are classified into two groups based on similar orbital distances: these are the Portia group, which includes the six moons Bianca, Cressida, Desdemona, Juliet, Portia, and Rosalind; and the Belinda group, which includes the three moons Cupid, Belinda, and Perdita.[13][23] Uranus XXVIII, which orbits between Ophelia and Bianca, is not classified into either of these groups.[24] 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.[25] 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.[13] 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.[26]

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%.[27] They are composed of water ice contaminated with a dark material, probably radiation-processed organics.[28]

The inner moons constantly perturb each other, especially within the closely-packed Portia and Belinda groups. The system is chaotic and apparently unstable.[29] Simulations show that the moons may perturb each other into crossing orbits, which may eventually result in collisions between the moons.[13] Desdemona may collide with Cressida within the next million years,[30] and Cupid will likely collide with Belinda in the next 10 million years; Perdita and Juliet may be involved in later collisions.[31] Because of this, the rings and inner moons may be under constant flux, with moons colliding and re-accreting on short timescales.[31]

### 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.[22] All these moons are relatively dark objects: their geometrical albedo varies between 30 and 50%, whereas their Bond albedo is between 10 and 23%.[27] 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 and a diameter of 3474 km.[32] 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.[33][34] This view is supported by their large thermal inertia, a surface property they share with dwarf planets like Pluto and Haumea.[35] It differs strongly from the thermal behaviour of the Uranian irregular moons that is comparable to classical trans-Neptunian objects.[36] 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.[37] The ice component may include ammonia and carbon dioxide.[38] 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.[3] Extensional processes associated with upwelling diapirs are likely responsible for the origin of the coronae.[39] Ariel appears to have the youngest surface with the fewest impact craters, while Umbriel's appears oldest.[3] 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.[40][41] 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.[42][43] The largest Uranian moons may be internally differentiated, with rocky cores at their centers surrounded by ice mantles.[37] Titania and Oberon may harbor liquid water oceans at the core/mantle boundary.[37] 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.[44]

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).[3] 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 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

See also: Astronomy:Irregular moon

Uranus's irregular moons range in size from 120 to 200 km (Sycorax) to under 10 km (S/2023 U 1).[45] Five of these moons have had their rotation periods measured, and on average, those in the Uranian system rotate faster than irregular moons around other giant planets.[36] This may reflect a history of more frequent or more energetic collisions within the Uranian system.[36]

Due to the small number of known Uranian irregular moons, it is not yet clear which of them belong to groups with similar orbital characteristics. The only known group among Uranus's irregular moons is the Caliban group, which is clustered at orbital distances between 6–7 million km (3.7–4.3 million mi) and inclinations between 141–144°.[15] The Caliban group includes three retrograde moons, which are Caliban, S/2023 U 1, and Stephano.[15] Beyond that, there is also a statistically significant division of its retrograde moons into two broad categories: those with smaller, more circular orbits and those with larger, more eccentric orbits.[4][46] However, the inclinations are distributed more or less randomly.[46]

Uranus is somewhat unique in that its retrograde moons do not orbit as far from the planet as those of the other giant planets, and only has one prograde irregular.[47] Margaret is the only known irregular prograde moon of Uranus, and it has one of the most eccentric orbits of any moon in the Solar System.

The intermediate inclinations 60° < i < 140° are devoid of known moons due to the Kozai instability.[4] 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.[4]

The orbits of Uranian irregular moons as seen from three different views. Prograde irregular moons are colored blue, retrograde irregular moons are colored red, and regular moons are colored magenta. Data as of 2026.

## List of moons

Orbital diagram of the orbital inclination and orbital distances for Uranus's rings and moon system at various scales. Open the image for full resolution.

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 10,000-year numerical integration by Sheppard et al. (2024). These may differ from osculating orbital elements provided by other sources.[47] The orbital elements of the inner moons listed here are based on the epoch of 1 January 2025; those for the major moons are based on the epoch of 1 January 2000; while orbital elements of irregular satellites are based on the epoch of 1 January 2020.[48][49]

Key  Inner moons (14) | ♠ Major moons (5) | ♦ Caliban group (3)

|
|

† Margaret (1)  | ‡ Ungrouped retrograde irregular moons (6)

Template:Sticky table start

Uranian moons  Label
[lower-alpha 4] | Name  | Pronunciation
(key)  | Image  | Abs.
magn.
[50] | Diameter
(km)
[lower-alpha 5] | Mass
(× 1016 kg)
[lower-alpha 6] | Semi-major axis
(km)
[lower-alpha 7] | Orbital period
(d)
[lower-alpha 7][lower-alpha 8] | Inclination
(°)
[lower-alpha 7][lower-alpha 9] | Eccentricity
[lower-alpha 7] | Discovery
year
[52] | Year announced  | Discoverer
[52] | Group

|
|
|
|
|
|
|
|
|
|
|
|
|
|

06 VI  | Cordelia | /kɔːrˈdiːliə/ | 50px | 10.3 | 0040 40 ± 6
(50 × 36) | 000006.08 6.08±0.57 | 49755 | 0.3347 +0.3347 | 0.2 | 0.000 | 1986 | 1986 | Terrile
(Voyager 2) | ε ring shepherd
07 VII  | Ophelia | /oʊˈfiːliə/ | 50px | 10.2 | 0043 43 ± 8
(54 × 38) | 000003.57 3.57±0.32 | 53765 | 0.3764 +0.3764 | 0.2 | 0.011 | 1986 | 1986 | Terrile
(Voyager 2) | ε ring shepherd
28 XXVIII | S/2025 U 1 |  | 50px | 13.6 ≈ 13.6  | 0005 ≈ 8–10  | 000000.04 ≈ 0.04  | 57844 | 0.4201 +0.4201 | 4.0 | 0.039 | 2025 | 2025 | El Moutamid et al.
(JWST) |
08 VIII  | Bianca | /biˈɑːŋkə/ | 50px | 9.8 | 0051 51 ± 4
(64 × 46) | 000006.9 ≈ 6.9  | 59170 | 0.4347 +0.4347 | 2.3 | 0.006 | 1986 | 1986 | Smith
(Voyager 2) | Portia
09 IX  | Cressida | /ˈkrɛsədə/ | 50px | 8.9 | 0080 80 ± 4
(92 × 74) | 000018.39 18.39±2.12 | 61770 | 0.4639 +0.4639 | 1.8 | 0.004 | 1986 | 1986 | Synnott
(Voyager 2) | Portia
10 X  | Desdemona | /ˌdɛzdəˈmoʊnə/ | 50px | 9.3 | 0064 64 ± 8
(90 × 54) | 000014 ≈ 14  | 62663 | 0.4736 +0.4736 | 3.1 | 0.007 | 1986 | 1986 | Synnott
(Voyager 2) | Portia
11 XI  | Juliet | /ˈdʒuːliət/ | 50px | 8.5 | 0094 94 ± 8
(150 × 74) | 000043 ≈ 43  | 64362 | 0.4931 +0.4931 | 3.0 | 0.006 | 1986 | 1986 | Synnott
(Voyager 2) | Portia
12 XII  | Portia | /ˈpɔːrʃə/ | 50px | 7.7 | 0135 135 ± 8
(156 × 126) | 000130 ≈ 130  | 66101 | 0.5132 +0.5132 | 2.7 | 0.004 | 1986 | 1986 | Synnott
(Voyager 2) | Portia
13 XIII  | Rosalind | /ˈrɒzələnd/ | 50px | 9.1 | 0072 72 ± 12  | 000020 ≈ 20  | 69930 | 0.5583 +0.5583 | 1.7 | 0.003 | 1986 | 1986 | Synnott
(Voyager 2) | Portia
27 XXVII  | Cupid | /ˈkjuːpəd/ | 50px | 12.6 | 0018 ≈ 18  | 000000.31 ≈ 0.31  | 74396 | 0.6125 +0.6125 | 2.0 | 0.007 | 2003 | 2003 | Showalter and
Lissauer (HST) | Belinda
14 XIV  | Belinda | /bəˈlɪndə/ |  | 8.8 | 0090 90 ± 16
(128 × 64) | 000038 ≈ 38  | 75258 | 0.6236 +0.6236 | 1.4 | 0.002 | 1986 | 1986 | Synnott
(Voyager 2) | Belinda
25 XXV  | Perdita | /ˈpɜːrdətə/ | 50px | 11.0 | 0030 30 ± 6  | 000001.4 ≈ 1.4  | 76418 | 0.6382 +0.6382 | 1.6 | 0.005 | 1999 | 1999 | Karkoschka
(Voyager 2) | Belinda
15 XV  | Puck | /ˈpʌk/ |  | 7.3 | 0162 162 ± 4  | 000191 191±64 | 86004 | 0.76183 +0.76183 | 0.327 | 0.0001 | 1985 | 1986 | Synnott
(Voyager 2) |
26 XXVI  | Mab | /ˈmæb/ |  | 12.1 | 0018 ≈ 18  | 000000.31 ≈ 0.31  | 97737 | 0.9229 +0.9229 | 1.8 | 0.006 | 2003 | 2003 | Showalter and
Lissauer (HST) | μ ring source
05 V  | Miranda♠ | /məˈrændə/ |  | 3.5 | 0470 471.6 ± 1.4
(481 × 468 × 466) | 006293 6293±300 | 129846 | 1.4135 +1.4135 | 4.421 | 0.0014 | 1948 | 1948 | Kuiper |
01 I  | Ariel♠ | /ˈɛəriɛl/ |  | 1.0 | 1157 1157.8±1.2
(1162 × 1156 × 1155) | 123310 123310±1800 | 190929 | 2.5204 +2.5204 | 0.026 | 0.0014 | 1851 | 1851 | Lassell |
02 II  | Umbriel♠ | /ˈʌmbriəl/ |  | 1.7 | 1169 1169.4±5.6 | 128850 128850±2250 | 265986 | 4.1442 +4.1442 | 0.083 | 0.0039 | 1851 | 1851 | Lassell |
03 III  | Titania♠ | /təˈtɑːniə/ |  | 0.8 | 1577 1576.8±1.2 | 345500 345500±5090 | 436298 | 8.7059 +8.7059 | 0.114 | 0.0016 | 1787 | 1787 | Herschel |
04 IV  | Oberon♠ | /ˈoʊbərɒn/ |  | 1.0 | 1522 1522.8±5.2 | 311040 311040±7490 | 583511 | 13.463 +13.463 | 0.125 | 0.0016 | 1787 | 1787 | Herschel |
22 XXII  | Francisco‡ | /frænˈsɪskoʊ/ | 50px | 12.9 | 0022 ≈ 22  | 000000.56 ≈ 0.56  | 4275700 | 267 −267 | 146.8 | 0.144 | 2001 | 2003 | Holman et al. |
16 XVI  | Caliban♦ | /ˈkæləbæn/ | 50px | 8.9 | 0042 42+20
−12 | 000003.9 ≈ 3.9  | 7167000 | 580 −580 | 141.4 | 0.200 | 1997 | 1997 | Gladman et al. | Caliban
20 XX  | Stephano♦ | /ˈstɛfənoʊ/ | 50px | 11.6 | 0032 ≈ 32  | 000001.7 ≈ 1.7  | 7951400 | 677 −677 | 143.6 | 0.235 | 1999 | 1999 | Gladman et al. | Caliban
99  | S/2023 U 1♦ |  |  | 13.7 | 0008 ≈ 8  | 000000.027 ≈ 0.027  | 7976600 | 681 −681 | 143.9 | 0.250 | 2023 | 2024 | Sheppard et al. | Caliban
21 XXI  | Trinculo‡ | /ˈtrɪŋkjʊloʊ/ | 50px | 12.7 | 0018 ≈ 18  | 000000.31 ≈ 0.31  | 8502600 | 749 −749 | 167.1 | 0.220 | 2001 | 2002 | Holman et al. |
17 XVII  | Sycorax‡ | /ˈsɪkəræks/ | 50px | 7.5 | 0157 157+23
−15 | 000200 ≈ 200  | 12193200 | 1286 −1286 | 157.0 | 0.520 | 1997 | 1997 | Nicholson et al. |
23 XXIII  | Margaret† | /ˈmɑːrɡərət/ | 50px | 12.7 | 0020 ≈ 20  | 000000.42 ≈ 0.42  | 14425000 | 1655 +1655 | 60.5 | 0.642 | 2003 | 2003 | Sheppard and
Jewitt |
18 XVIII  | Prospero‡ | /ˈprɒspəroʊ/ | 50px | 10.6 | 0050 ≈ 50  | 000006.5 ≈ 6.5  | 16221000 | 1974 −1974 | 149.4 | 0.441 | 1999 | 1999 | Holman et al. |
19 XIX  | Setebos‡ | /ˈsɛtɛbʌs/ | 50px | 10.6 | 0047 ≈ 47  | 000005.4 ≈ 5.4  | 17519800 | 2215 −2215 | 153.9 | 0.579 | 1999 | 1999 | Kavelaars et al. |
24 XXIV  | Ferdinand‡ | /ˈfɜːrdənænd/ | 50px | 12.4 | 0021 ≈ 21  | 000000.48 ≈ 0.48  | 20421400 | 2788 −2788 | 169.2 | 0.395 | 2001 | 2003 | Holman et al. |

Template:Sticky table end

## See also

* List of natural satellites

## Notes

1. ↑ The mass of Triton is about 2.14 × 1022 kg,[21] 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°.[3]
4. ↑ Label refers to the Roman numeral attributed to each moon in order of their discovery.[2]
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.[22] The diameter of Titania is from Widemann, 2009.[44] The dimensions and radii of the inner moons are from Karkoschka, 2001,[12] except for Cupid, Mab, and Uranus XXVIII. The radii of Cupid and Mab were taken from Showalter, 2006.[13] The dimensions of Uranus XXVIII are a calculated estimate. The radii of outer moons except Sycorax, Caliban, and S/2023 U 1 were taken from Sheppard's website.[45] The radii of Sycorax and Caliban are from Farkas-Takács et al., 2017.[36] The dimensions of S/2023 U 1 are a calculated estimate.
6. ↑ Masses of Puck, Miranda, Ariel, Umbriel, Titania, and Oberon were taken from Jacobson & Park, 2025.[48] Masses of Cordelia, Ophelia, and Cressida were taken from French, 2024.[51] Masses of all other moons were calculated assuming a density of 1 g/cm3 and using given radii.
7. ↑ 7.0 7.1 7.2 7.3 Mean orbits of the inner and irregular satellites, other than Puck, are taken from JPL Small System Dynamics,[49] while mean orbits of the five major moons and Puck are taken from Jacobson & Park (2025).[48]
8. ↑ Negative orbital periods indicate a retrograde orbit around Uranus (opposite to the planet's orbit). Orbital periods of irregular satellites may not be consistent with their semi-major axes due to perturbations.
9. ↑ Inclinations greater than 90° are retrograde. Orbital inclinations of inner satellites, other than Puck, are with respect to their Laplace planes. For the major satellites and Puck, inclination measures the angle between the moon's orbital plane and the plane defined by Uranus's equator. For irregular satellites, inclination measures the angle between the moon's orbital plane and the ecliptic.

## References

1. ↑ 1.0 1.1 El Moutamid, Maryame (2025-08-19). "New Moon Discovered Orbiting Uranus Using NASA's Webb Telescope". NASA. https://science.nasa.gov/blogs/webb/2025/08/19/new-moon-discovered-orbiting-uranus-using-nasas-webb-telescope/. Retrieved 2025-08-19.
2. ↑ 2.0 2.1 2.2 "Planet and Satellite Names and Discoverers". Gazetteer of Planetary Nomenclature. USGS Astrogeology. 21 July 2006. https://planetarynames.wr.usgs.gov/Page/Planets.
3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 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. Retrieved 28 June 2019.
4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 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.
5. ↑ 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.
6. ↑ 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.
7. ↑ 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.
8. ↑ 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.
9. ↑ 9.0 9.1 9.2 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.
10. ↑ Kaempffert, Waldemar (26 December 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.
11. ↑ 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.
12. ↑ 12.0 12.1 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.
13. ↑ 13.0 13.1 13.2 13.3 13.4 13.5 Showalter, Mark R.; Lissauer, Jack J. (2006-02-17). "The Second Ring-Moon System of Uranus: Discovery and Dynamics". Science 311 (5763): 973–977. doi:10.1126/science.1122882. PMID 16373533. Bibcode: 2006Sci...311..973S.
14. ↑ "MPEC 2024-D113 : S/2023 U 1". Minor Planet Electronic Circular. Minor Planet Center. 23 February 2024. https://minorplanetcenter.net/mpec/K24/K24DB3.html. Retrieved 23 February 2024.
15. ↑ 15.0 15.1 15.2 "New Uranus and Neptune Moons". Earth & Planetary Laboratory. Carnegie Institution for Science. 23 February 2024. https://sites.google.com/carnegiescience.edu/sheppard/home/newuranusneptunemoons. Retrieved 23 February 2024.
16. ↑ "Scientists Discover a New Moon Orbiting Uranus". The New York Times. 2025-08-20. https://www.nytimes.com/2025/08/20/science/uranus-new-moon.html.
17. ↑ 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.
18. ↑ Denning, W.F. (22 October 1881). "The centenary of the discovery of Uranus". Scientific American Supplement (303). http://www.infomotions.com/etexts/gutenberg/dirs/etext05/7030310.htm.
19. ↑ William Lassell (1852). "Beobachtungen der Uranus-Satelliten". Astronomische Nachrichten 34: 325. Bibcode: 1852AN.....34..325..
20. ↑ 20.0 20.1 Paul, Richard (2014). "The Shakespearean Moons of Uranus". Folger Shakespeare Library. https://www.folger.edu/podcasts/shakespeare-unlimited/shakespearean-moons-uranus/.
21. ↑ 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.
22. ↑ 22.0 22.1 22.2 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.
23. ↑ Ćuk, Matija; French, Robert S.; Showalter, Mark R.; Tiscareno, Matthew S.; El Moutamid, Maryame (August 2022). "Cupid is not Doomed Yet: On the Stability of the Inner Moons of Uranus". The Astronomical Journal 164 (2): 8. doi:10.3847/1538-3881/ac745d. 38. Bibcode: 2022AJ....164...38C.
24. ↑ Green, Daniel W. E. (19 August 2025). "CBET 5593: S/2025 U 1". Central Bureau Electronic Telegram. Central Bureau for Astronomical Telegrams. http://www.cbat.eps.harvard.edu/iau/cbet/005500/CBET005593.txt. Retrieved 19 August 2025.
25. ↑ 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.
26. ↑ 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.
27. ↑ 27.0 27.1 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.
28. ↑ 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.
29. ↑ 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.
30. ↑ "Uranus's colliding moons". astronomy.com. 2017. http://www.astronomy.com/news/2017/09/uranus-colliding-moons.
31. ↑ 31.0 31.1 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.
32. ↑ 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.
33. ↑ 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.
34. ↑ 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.
35. ↑ 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.
36. ↑ 36.0 36.1 36.2 36.3 Farkas-Takács, A. et al. (September 2017). "Properties of the Irregular Satellite System around Uranus Inferred from K2, Herschel, and Spitzer Observations". The Astronomical Journal 154 (3): 119–131. doi:10.3847/1538-3881/aa8365. ISSN 1538-3881. Bibcode: 2017AJ....154..119F.
37. ↑ 37.0 37.1 37.2 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.
38. ↑ 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.
39. ↑ 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.
40. ↑ 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.
41. ↑ 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.
42. ↑ 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. Retrieved 2011-01-25.
43. ↑ 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.
44. ↑ 44.0 44.1 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.
45. ↑ 45.0 45.1 Sheppard, Scott S.. "Moons of Uranus". Earth & Planets Laboratory. Carnegie Institution for Science. https://sites.google.com/carnegiescience.edu/sheppard/moons/uranusmoons. Retrieved 23 February 2024.
46. ↑ 46.0 46.1 Nicholson, Philip D.; Ćuk, Matija; Sheppard, Scott S.; Nesvorný, David; Johnson, Torrence V. (May 8, 2008). "Irregular Satellites of the Giant Planets". in Barucci, M. Antonietta. The Solar System Beyond Neptune. The University of Arizona Space Science. University of Arizona Press. ISBN 978-0816527557. Bibcode: 2008ssbn.book..411N. https://web.gps.caltech.edu/~mbrown/out/kbbook/Chapters/Nicholson_IrregSat.pdf.
47. ↑ 47.0 47.1 Sheppard, Scott S.; Tholen, David J.; Brozovic, Marina; Jacobson, Robert; Trujillo, Chadwick A.; Lykawka, Patryk Sofia; Alexandersen, Mike (2024-12-01). "New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys". The Astronomical Journal 168 (6): 258. doi:10.3847/1538-3881/ad7fed. ISSN 0004-6256. Bibcode: 2024AJ....168..258S.
48. ↑ 48.0 48.1 48.2 Jacobson, Robert A.; Park, Ryan S. (2025-02-03). "The Orbits of Uranus, Its Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Poles of Uranus and Its Satellites". The Astronomical Journal 169 (2): 65. doi:10.3847/1538-3881/ad99d1. ISSN 0004-6256. Bibcode: 2025AJ....169...65J.
49. ↑ 49.0 49.1 "Planetary Satellite Mean Elements". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sats/elem/. Retrieved 9 November 2025.
50. ↑ "Natural Satellites Ephemeris Service". IAU: Minor Planet Center. https://minorplanetcenter.org/iau/NatSats/NaturalSatellites.html.
51. ↑ French, Richard G.; Hedman, Matthew M.; Nicholson, Philip D.; Longaretti, Pierre-Yves; McGhee-French, Colleen A. (March 2024). "The Uranus system from occultation observations (1977–2006): Rings, pole direction, gravity field, and masses of Cressida, Cordelia, and Ophelia". Icarus 411. doi:10.1016/j.icarus.2024.115957. Bibcode: 2024Icar..41115957F.
52. ↑ 52.0 52.1 "Planetary Satellite Discovery Circumstances". JPL Solar System Dynamics. NASA. https://ssd.jpl.nasa.gov/sats/discovery.html. Retrieved 28 February 2024.

## External links

* Scott S. Sheppard: Uranus Moons
* Simulation Showing the location of Uranus's Moons
* "Uranus: Moons". NASA's Solar System Exploration. http://solarsystem.nasa.gov/planets/uranus/moons.
* "NASA's Hubble Discovers New Rings and Moons Around Uranus". Space Telescope Science Institute. 22 December 2005. http://hubblesite.org/news_release/news/2005-33.
* Gazetteer of Planetary Nomenclature—Uranus (USGS)
* Uranus Rings photos, NASA, December 18, 2023, https://webbtelescope.org/contents/news-releases/2023/news-2023-150, retrieved 19 December 2023

* v
* t
* e

Moons of Uranus

* Generally listed in increasing distance from Uranus

Inner|

* Rings of Uranus
* Cordelia
* Ophelia
* Bianca
* Cressida
* Desdemona
* Juliet
* Portia
* Rosalind
* Cupid
* Belinda
* Perdita
* Puck
* Mab

Major (spheroid)|

* Miranda
* Ariel
* Umbriel
* Titania
* Oberon

Outer (irregular)|

* Francisco
* Caliban
* Stephano
* Trinculo
* Sycorax
* Margaret
* Prospero
* Setebos
* Ferdinand

Geological features|

* Arielian
* Kachina Chasmata
* Yangoor
* Mirandian
* Verona Rupes
* Oberonian
* Hamlet
* Mommur Chasma
* Puckian
* Titanian
* Gertrude
* Messina Chasmata
* Ursula
* Rousillon Rupes
* Umbrielian
* Wunda
* Vuver
* Skynd

* v
* t
* e

Uranus (Outline of Uranus

Geography|

* Atmosphere
* Climate
* Dark Spot
* Magnetosphere
* Rings

NASA image of Uranus

Moons|

* Ariel
* Miranda
* Oberon
* Puck
* Titania
* Umbriel

Astronomy|

| Discovery|

* William Herschel
* Gerard Kuiper
* James L. Elliot
* William Lassell

|

General|

* 15 Orionis
* Uranus-crossing minor planets

Trojans|

* 2011 QF99
* 2014 YX49

Exploration|

| Past|

* Voyager 2 (1986 flyby)

|

Proposals|

* MUSE
* Oceanus
* ODINUS
* NASA Uranus orbiter and probe
* Uranus Pathfinder

Related|

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Natural satellites of the Solar System

Planetary
satellites|

* Terrestrial
* Martian
* Jovian
* Saturnian
* Uranian
* Neptunian

Dwarf-planet
satellites|

* Plutonian
* Haumean
* Makemakean
* Eridian
* OR10
* Quaoaran
* Orcean

Minor-planet moons|

* Main belt binaries:
* Antiope
* Frostia
* Berna
* Tokai
* Ostro
* Balam
* Doppler
* Pauling
* Iwamoto
* Wolff
* Bettig
* Christophedumas
* Trojans:
* Patroclus–Menoetius
* Hektor–Skamandrios
* Iphthime
* Eurydamas
* TNOs:
* Huya
* Typhon–Echidna
* Lempo–Paha–Hiisi
* 2002 UX25
* Logos–Zoe
* Ceto–Phorcys
* Borasisi–Pabu
* Sila–Nunam
* Teharonhiawako–Sawiskera
* Salacia–Actaea
* 2002 WC19
* Altjira
* Varda–Ilmarë
* 2003 AZ84
* Gǃkúnǁʼhòmdímà–Gǃòʼé ǃHú
* Mors–Somnus
* Manwë–Thorondor
* ǂKá̦gára–ǃHãunu
* 2013 FY27

Ranked by size|

* Planetary-mass moon
* Ganymede
* largest: 5268 km / 0.413 Earths
* Titan
* Callisto
* Io
* Moon
* Europa
* Triton
* Titania
* Rhea
* Oberon
* Iapetus
* Charon
* Umbriel
* Ariel
* Dione
* Tethys
* Dysnomia
* Enceladus
* Miranda
* Vanth
* Proteus
* Mimas
* Ilmarë
* Nereid
* Hiʻiaka
* Actaea
* Hyperion
* ...

* Discovery timeline
* Inner moons
* Irregular moons
* List
* Planetary-mass moons
* Naming
* Subsatellite
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* Trojan moons

* v
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* e

Solar System

* Sun
* Mercury
* Venus
* Earth
* Mars
* Ceres
* Jupiter
* Saturn
* Uranus
* Neptune
* Pluto
* Haumea
* Makemake
* Eris

| Planets|

* Terrestrial planets
* Mercury
* Venus
* Earth
* Mars

* Giant planets
* Jupiter
* Saturn
* Uranus
* Neptune

* Dwarf planets
* Ceres
* Pluto
* Haumea
* Makemake
* Eris

|

Rings|

* Jovian
* Saturnian (Rhean)
* Charikloan
* Chironean
* Uranian
* Neptunian
* Haumean

Moons|

* Terrestrial
* Moon
* other near-Earth objects
* Martian
* Phobos
* Deimos
* Jovian
* Ganymede
* Callisto
* Io
* Europa
* all 79
* Saturnian
* Titan
* Rhea
* Iapetus
* Dione
* Tethys
* Enceladus
* Mimas
* Hyperion
* Phoebe
* all 82
* Uranian
* Titania
* Oberon
* Umbriel
* Ariel
* Miranda
* all 27
* Neptunian
* Triton
* Proteus
* Nereid
* all 14
* Plutonian
* Charon
* Nix
* Hydra
* Kerberos
* Styx
* Eridian
* Dysnomia
* Haumean
* Hiʻiaka
* Namaka
* Makemakean
* S/2015 (136472) 1

Exploration
(outline)|

* Colonization
* Discovery
* astronomy
* historical models
* timeline
* Human spaceflight
* space stations
* list
* Space probes
* timeline
* list

* Mercury
* Venus
* Moon
* mining
* Mars
* Ceres
* Asteroids
* mining
* Comets
* Jupiter
* Saturn
* Uranus
* Neptune
* Pluto
* Deep space

Hypothetical
objects|

* Fifth giant
* Nemesis
* Phaeton
* Planet Nine
* Planet V
* Planet X
* Theia
* Tyche
* Vulcan
* Vulcanoids
* Subsatellites

Lists|

* Comets
* Dwarf planets (possible)
* Gravitationally rounded objects
* Minor planets
* names
* Natural satellites
* Solar System models
* Solar System objects
* by size
* by discovery date

| Small Solar
System bodies|

* Comets
* Damocloids
* Meteoroids
* Minor planets
* moons
* Planetesimal

* Mercury-crossers
* Venus-crossers
* Venus trojans
* Near-Earth objects
* Earth-crossers
* Earth trojans
* Mars-crossers
* Mars trojans

* Asteroid belt
* Asteroids
* Ceres
* Pallas
* Juno
* Vesta
* first 1000
* families
* exceptional
* Kirkwood gap
* Main-belt comets

* Jupiter-crossers
* Jupiter trojans
* Centaurs
* Saturn-crossers
* Uranus-crossers
* Uranus trojans
* Neptune-crossers
* Neptune trojans
* Cis-Neptunian objects
* Trans-Neptunian objects

* Plutoids
* Kuiper belt
* Cubewanos
* Plutinos
* Detached objects
* Hills cloud
* Oort cloud
* Scattered disc
* Sednoids

|

Formation
and evolution|

* Accretion
* Accretion disk
* Asteroid belt
* Circumplanetary disk
* Circumstellar disc
* Circumstellar envelope
* Cosmic dust
* Debris disk
* Detached object
* Disrupted planet
* Excretion disk
* Exoplanetary Circumstellar Environments and Disk Explorer
* Exozodiacal dust
* Extraterrestrial materials
* Extraterrestrial sample curation
* Giant-impact hypothesis
* Gravitational collapse
* Hills cloud
* Interplanetary dust cloud
* Interplanetary medium
* Interplanetary space
* Interstellar cloud
* Interstellar dust
* Interstellar medium
* Interstellar space
* Kuiper belt
* List of interstellar and circumstellar molecules
* Merging stars
* Molecular cloud
* Nebular hypothesis
* Oort cloud
* Outer space
* Planetary migration
* Planetary system
* Planetesimal
* Planet formation
* Protoplanetary disk
* Ring system
* Rubble pile
* Sample-return mission
* Scattered disc
* Star formation

* Outline of the Solar System
*   *   *

Solar System → Local Interstellar Cloud → Local Bubble → Gould Belt → Orion Arm → Milky Way → Milky Way subgroup → Local Group → Local Sheet → Virgo Supercluster → Laniakea Supercluster → Observable universe → Universe
Each arrow (→) may be read as "within" or "part of".

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