Moons of Neptune

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An annotated picture of some of Neptune's many moons as captured by the James Webb Space Telescope. The bright blue diffraction star is Triton, Neptune's largest moon; while Hippocamp, its smallest regular moon, is too small to be seen. New Webb Images Capture Rare View of Neptune's Rings (Labeled).png
An annotated picture of some of Neptune's many moons as captured by the James Webb Space Telescope. The bright blue diffraction star is Triton, Neptune's largest moon; while Hippocamp, its smallest regular moon, is too small to be seen.

The planet Neptune has 16 known moons, which are named for minor water deities and a water creature in Greek mythology. By far the largest of them is Triton, discovered by William Lassell on October 10, 1846, 17 days after the discovery of Neptune itself. Over a century passed before the discovery of the second natural satellite, Nereid, in 1949, and another 40 years passed before Proteus, Neptune's second-largest moon, was discovered in 1989.

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Triton is unique among moons of planetary mass in that its orbit is retrograde to Neptune's rotation and inclined relative to Neptune's equator, which suggests that it did not form in orbit around Neptune but was instead gravitationally captured by it. The next-largest satellite in the Solar System suspected to be captured, Saturn's moon Phoebe, has only 0.03% of Triton's mass. The capture of Triton, probably occurring some time after Neptune formed a satellite system, was a catastrophic event for Neptune's original satellites, disrupting their orbits so that they collided to form a rubble disc. Triton is massive enough to have achieved hydrostatic equilibrium and to retain a thin atmosphere capable of forming clouds and hazes.

Inward of Triton are seven small regular satellites, all of which have prograde orbits in planes that lie close to Neptune's equatorial plane; some of these orbit among Neptune's rings. The largest of them is Proteus. They were re-accreted from the rubble disc generated after Triton's capture after the Tritonian orbit became circular. Neptune also has eight more outer irregular satellites other than Triton, including Nereid, whose orbits are much farther from Neptune and at high inclination: three of these have prograde orbits, while the remainder have retrograde orbits. In particular, Nereid has an unusually close and eccentric orbit for an irregular satellite, suggesting that it may have once been a regular satellite that was significantly perturbed to its current position when Triton was captured. Neptune's outermost moon S/2021 N 1, which has an orbital period of about 27 Earth years, orbits farther from its planet than any other known moon in the Solar System. [1] [2]

History

Discovery

Triton was discovered by William Lassell in 1846, just seventeen days after the discovery of Neptune. [3] Nereid was discovered by Gerard P. Kuiper in 1949. [4] The third moon, later named Larissa, was first observed by Harold J. Reitsema, William B. Hubbard, Larry A. Lebofsky and David J. Tholen on May 24, 1981. The astronomers were observing a star's close approach to Neptune, looking for rings similar to those discovered around Uranus four years earlier. [5] If rings were present, the star's luminosity would decrease slightly just before the planet's closest approach. The star's luminosity dipped only for several seconds, which meant that it was due to a moon rather than a ring.

No further moons were found until Voyager 2 flew by Neptune in 1989. Voyager 2 rediscovered Larissa and discovered five inner moons: Naiad, Thalassa, Despina, Galatea and Proteus. [6] In 2001, two surveys using large ground-based telescopes found five additional outer irregular moons, bringing the total to thirteen. [7] Follow-up surveys by two teams in 2002 and 2003 respectively re-observed all five of these moons, which are Halimede, Sao, Psamathe, Laomedeia, and Neso. [7] [8] The 2002 survey also found a sixth moon, but it could not be re-observed enough times to determine its orbit, and it thus became lost. [7]

In 2013 Mark R. Showalter discovered Hippocamp while examining Hubble Space Telescope images of Neptune's ring arcs from 2009. He used a technique similar to panning to compensate for orbital motion and allow stacking of multiple images to bring out faint details. [9] [10] After deciding on a whim to expand the search area to radii well beyond the rings, he found an unambiguous dot that represented the new moon. [11] He then found it repeatedly in other archival HST images going back to 2004. Voyager 2, which had observed all of Neptune's other inner satellites, did not detect it during its 1989 flyby, due to its dimness. [9]

In 2021, Scott S. Sheppard and colleagues used the Subaru Telescope at Mauna Kea, Hawaii and discovered two more irregular moons of Neptune, which were announced in 2024. [12] These two moons are provisionally designated S/2021 N 1 and S/2002 N 5. The latter turned out to be a recovery of the lost moon from 2002. [2] [13]

Discovery of outer planet moons

   Moons of Jupiter
   Moons of Saturn
   Moons of Uranus

Names

Triton did not have an official name until the twentieth century. The name "Triton" was suggested by Camille Flammarion in his 1880 book Astronomie Populaire, [14] but it did not come into common use until at least the 1930s. [15] Until this time it was usually simply known as "the satellite of Neptune". Other moons of Neptune are also named for Greek and Roman water gods, in keeping with Neptune's position as god of the sea: [16] either from Greek mythology, usually children of Poseidon, the Greek Neptune (Triton, Proteus, Despina, Thalassa); lovers of Poseidon (Larissa); other mythological creatures related to Poseidon (Hippocamp); classes of minor Greek water deities (Naiad, Nereid); or specific Nereids (Halimede, Galatea, Neso, Sao, Laomedeia, Psamathe). [16] [17]

For the "normal" irregular satellites, the general convention is to use names ending in "a" for prograde satellites, names ending in "e" for retrograde satellites, and names ending in "o" for exceptionally inclined satellites, exactly like the convention for the moons of Jupiter. [18] Two asteroids share the same names as moons of Neptune: 74 Galatea and 1162 Larissa.

Characteristics

The moons of Neptune can be divided into two groups: regular and irregular. The first group includes the seven inner moons, which follow circular prograde orbits lying in the equatorial plane of Neptune. The second group consists of all nine other moons including Triton. They generally follow inclined eccentric and often retrograde orbits far from Neptune; the only exception is Triton, which orbits close to the planet following a circular orbit, though retrograde and inclined. [19]

Orbit diagram of Neptune's inner moons including Triton, with their names and orbit directions indicated Orbits of inner moons of Neptune including S 2004 N 1.jpg
Orbit diagram of Neptune's inner moons including Triton, with their names and orbit directions indicated
Size comparison of Neptune's seven inner moons Neptune inner moons size comparison.jpg
Size comparison of Neptune's seven inner moons

Regular moons

In order of distance from Neptune, the regular moons are Naiad, Thalassa, Despina, Galatea, Larissa, Hippocamp, and Proteus. All but the outer two are within Neptune-synchronous orbit (Neptune's rotational period is 0.6713 day or 16 hours [20] ) and thus are being tidally decelerated. Naiad, the closest regular moon, is also the second smallest among the inner moons (following the discovery of Hippocamp), whereas Proteus is the largest regular moon and the second largest moon of Neptune. The first five moons orbit much faster than Neptune's rotation itself ranging from 7 hours for Naiad and Thalassa, to 13 hours for Larissa.

The inner moons are closely associated with Neptune's rings. The two innermost satellites, Naiad and Thalassa, orbit between the Galle and LeVerrier rings. [6] Despina may be a shepherd moon of the LeVerrier ring, because its orbit lies just inside this ring. [21] The next moon, Galatea, orbits just inside the most prominent of Neptune's rings, the Adams ring. [21] This ring is very narrow, with a width not exceeding 50 km, [22] and has five embedded bright arcs. [21] The gravity of Galatea helps confine the ring particles within a limited region in the radial direction, maintaining the narrow ring. Various resonances between the ring particles and Galatea may also have a role in maintaining the arcs. [21]

Only the two largest regular moons have been imaged with a resolution sufficient to discern their shapes and surface features. [6] Larissa, about 200 km in diameter, is elongated. Proteus is not significantly elongated, but not fully spherical either: [6] it resembles an irregular polyhedron, with several flat or slightly concave facets 150 to 250 km in diameter. [23] At about 400 km in diameter, it is larger than the Saturnian moon Mimas, which is fully ellipsoidal. This difference may be due to a past collisional disruption of Proteus. [24] The surface of Proteus is heavily cratered and shows a number of linear features. Its largest crater, Pharos, is more than 150 km in diameter. [6] [23]

All of Neptune's inner moons are dark objects: their geometric albedo ranges from 7 to 10%. [25] Their spectra indicate that they are made from water ice contaminated by some very dark material, probably complex organic compounds. In this respect, the inner Neptunian moons are similar to the inner Uranian moons. [6]

Irregular moons

The orbit of Triton (red) is different from most moons' orbit (green) in the orbit's direction, and the orbit is tilted -23deg. Triton orbit & Neptune.png
The orbit of Triton (red) is different from most moons' orbit (green) in the orbit's direction, and the orbit is tilted −23°.

In order of their distance from the planet, the irregular moons are Triton, Nereid, Halimede, Sao, S/2002 N 5, Laomedeia, Psamathe, Neso, and S/2021 N 1, a group that includes both prograde and retrograde objects. [19] The seven outermost moons are similar to the irregular moons of other giant planets, and are thought to have been gravitationally captured by Neptune, unlike the regular satellites, which probably formed in situ . [8]

Triton and Nereid are unusual irregular satellites and are thus treated separately from the other seven irregular Neptunian moons, which are more like the outer irregular satellites of the other outer planets. [8] Firstly, they are the largest two known irregular moons in the Solar System, with Triton being almost an order of magnitude larger than all other known irregular moons. Secondly, they both have atypically small semi-major axes, with Triton's being over an order of magnitude smaller than those of all other known irregular moons. Thirdly, they both have unusual orbital eccentricities: Nereid has one of the most eccentric orbits of any known irregular satellite, and Triton's orbit is a nearly perfect circle. Finally, Nereid also has the lowest inclination of any known irregular satellite. [8]

Triton

Irregular satellites of Jupiter (red), Saturn (green), Uranus (magenta) and Neptune (blue; including Triton), plotted by distance from their planet (semi-major axis) in the horizontal axis and orbital inclination in the vertical axis. The semi-major axis values are expressed as a fraction of the planet's Hill sphere's radius, while the inclination is expressed in degrees from the ecliptic. The relative sizes of moons are indicated by the size of their symbols, and the Sao and Neso groups of Neptunian moons are labeled. Data as of February 2024. Irregular moon orbits a vs. i.jpg
Irregular satellites of Jupiter (red), Saturn (green), Uranus (magenta) and Neptune (blue; including Triton), plotted by distance from their planet (semi-major axis) in the horizontal axis and orbital inclination in the vertical axis. The semi-major axis values are expressed as a fraction of the planet's Hill sphere's radius, while the inclination is expressed in degrees from the ecliptic. The relative sizes of moons are indicated by the size of their symbols, and the Sao and Neso groups of Neptunian moons are labeled. Data as of February 2024.

Triton follows a retrograde and quasi-circular orbit, and is thought to be a gravitationally captured satellite. It was the second moon in the Solar System that was discovered to have a substantial atmosphere, which is primarily nitrogen with small amounts of methane and carbon monoxide. [26] The pressure on Triton's surface is about 14  μbar. [26] In 1989 the Voyager 2 spacecraft observed what appeared to be clouds and hazes in this thin atmosphere. [6] Triton is one of the coldest bodies in the Solar System, with a surface temperature of about 38 K (−235.2 °C). [26] Its surface is covered by nitrogen, methane, carbon dioxide and water ices [27] and has a high geometric albedo of more than 70%. [6] The Bond albedo is even higher, reaching up to 90%. [6] [note 1] Surface features include the large southern polar cap, older cratered planes cross-cut by graben and scarps, as well as youthful features probably formed by endogenic processes like cryovolcanism. [6] Voyager 2 observations revealed a number of active geysers within the polar cap heated by the Sun, which eject plumes to the height of up to 8 km. [6] Triton has a relatively high density of about 2 g/cm3 indicating that rocks constitute about two thirds of its mass, and ices (mainly water ice) the remaining one third. There may be a layer of liquid water deep inside Triton, forming a subterranean ocean. [28] Because of its retrograde orbit and relative proximity to Neptune (closer than the Moon is to Earth), tidal deceleration is causing Triton to spiral inward, which will lead to its destruction in about 3.6 billion years. [29]

Nereid

Nereid is the third-largest moon of Neptune. It has a prograde but very eccentric orbit and is believed to be a former regular satellite that was scattered to its current orbit through gravitational interactions during Triton's capture. [30] Water ice has been spectroscopically detected on its surface. Early measurements of Nereid showed large, irregular variations in its visible magnitude, which were speculated to be caused by forced precession or chaotic rotation combined with an elongated shape and bright or dark spots on the surface. [31] This was disproved in 2016, when observations from the Kepler space telescope showed only minor variations. Thermal modeling based on infrared observations from the Spitzer and Herschel space telescopes suggest that Nereid is only moderately elongated which disfavours forced precession of the rotation. [32] The thermal model also indicates that the surface roughness of Nereid is very high, likely similar to the Saturnian moon Hyperion. [32]

Nereid dominates the normal irregular satellites of Neptune, having about 98% of the mass of Neptune's entire irregular satellite system altogether (if Triton is not counted). This is similar to the situation of Phoebe at Saturn. If it is counted as a normal irregular satellite (but not Triton), then Nereid is also by far the largest normal irregular satellite known, having about two-thirds the mass of all normal irregular moons combined. [33]

Normal irregular moons

Among the remaining irregular moons, Sao, S/2002 N 5, and Laomedeia follow prograde orbits, whereas Halimede, Psamathe, Neso and S/2021 N 1 follow retrograde orbits. There are at least two groups of moons that share similar orbits, with the prograde moons Sao, S/2002 N 5, and Laomedeia belonging to the Sao group and the retrograde moons Psamathe, Neso, and S/2021 N 1 belonging to the Neso group. [12] The moons of the Neso group have the largest orbits of any natural satellites discovered in the Solar System to date, with average orbital distances over 125 times the distance between Earth and the Moon and orbital periods over 25 years. [34] Neptune has the largest Hill sphere in the Solar System, owing primarily to its large distance from the Sun; this allows it to retain control of such distant moons. [19] Nevertheless, the Jovian moons in the Carme and Pasiphae groups orbit at a greater percentage of their primary's Hill radius than the Neso group moons. [19]

Formation

The mass distribution of the Neptunian moons is the most lopsided of the satellite systems of the giant planets in the Solar System. One moon, Triton, makes up nearly all of the mass of the system, with all other moons together comprising only one third of one percent. This is similar to the moon system of Saturn, where Titan makes up more than 95% of the total mass, but is different from the more balanced systems of Jupiter and Uranus. The reason for the lopsidedness of the present Neptunian system is that Triton was captured well after the formation of Neptune's original satellite system, and experts conjecture much of the system was destroyed in the process of capture. [30] [35]

The relative masses of the Neptunian moons Masa de triton.svg
The relative masses of the Neptunian moons

Triton's orbit upon capture would have been highly eccentric, and would have caused chaotic perturbations in the orbits of the original inner Neptunian satellites, causing them to collide and reduce to a disc of rubble. [30] This means it is likely that Neptune's present inner satellites are not the original bodies that formed with Neptune. Only after Triton's orbit became circularised could some of the rubble re-accrete into the present-day regular moons. [24]

The mechanism of Triton's capture has been the subject of several theories over the years. One of them postulates that Triton was captured in a three-body encounter. In this scenario, Triton is the surviving member of a binary Kuiper belt object [note 2] disrupted by its encounter with Neptune. [36]

Numerical simulations show that there is a 0.41 probability that the moon Halimede collided with Nereid at some time in the past. [7] Although it is not known whether any collision has taken place, both moons appear to have similar ("grey") colors, implying that Halimede could be a fragment of Nereid. [37]

List

Orbital diagram of the orbital inclination and orbital distances for Neptune's rings and moon system at various scales. Notable moons and rings are individually labeled. Open the image for full resolution. Neptunemoonsdiagram.png
Orbital diagram of the orbital inclination and orbital distances for Neptune's rings and moon system at various scales. Notable moons and rings are individually labeled. Open the image for full resolution.

The Neptunian moons are listed here by orbital period, from shortest to longest. Irregular (captured) moons are marked by color. 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 30,000-year period: these may differ from osculating orbital elements provided by other sources. [38] Their orbital elements are all based on the epoch of 1 January 2020. [1] Triton, the only Neptunian moon massive enough for its surface to have collapsed into a spheroid, is emboldened.

Key
 
Inner moons		♠
Triton		†
Nereid		‡
Halimede		♦
Sao group		♥
Neso group
Neptunian moons
Label
[note 3] 		NamePronunciation
(key)		Image Abs.
magn. 		Diameter
(km) [note 4] 		Mass
(×1016 kg)
[note 5] 		Semi-major axis
(km) [17] 		Orbital period
(d) [1] 		Orbital inclination
(°) [1] 		Eccentricity
[17] [note 6] 		Discovery
year [16] 		Year announcedDiscoverer
[16] 		Group
III Naiad /ˈneɪəd,ˈnaɪæd/ [42]
Naiad Voyager.png
9.660.4
(96 × 60 × 52)		≈ 1348224+0.29444.6910.004719891989Voyager Science Teaminner
IV Thalassa /θəˈlæsə/
Neptune Trio.jpg
8.781.4
(108 × 100 × 52)		≈ 3550074+0.31150.1350.001819891989Voyager Science Teaminner
V Despina /dəˈspaɪnə/
Despina.jpg
7.3156
(180 × 148 × 128)		≈ 17052526+0.33460.0680.000419891989Voyager Science Teaminner
VI Galatea /ˌɡæləˈtiːə/
Galatea moon.jpg
7.2174.8
(204 × 184 × 144)		≈ 28061953+0.42870.0340.000119891989Voyager Science Teaminner
VII Larissa /ləˈrɪsə/
Larissa 1.jpg
6.8194
(216 × 204 × 168)		≈ 38073548+0.55550.2050.001219811981Reitsema et al.inner
XIV Hippocamp /ˈhɪpəkæmp/
Hippocamp-heic1904b.jpg
10.534.8±4.0≈ 2.2105283+0.95000.0640.000520132013 Showalter et al.inner
VIII Proteus /ˈproʊtiəs/
Proteus (Voyager 2).jpg
5.0420
(436 × 416 × 402)		≈ 3900117646+1.12230.0750.000519891989Voyager Science Teaminner
I Triton ♠ /ˈtraɪtən/
Neptune's Moon Triton Fosters Rare Icy Union (gemini1903a) (square crop).jpg
–1.22705.2±4.8
(2709 × 2706 × 2705)		2139000354759−5.8769156.8650.000018461846 Lassell
II Nereid † /ˈnɪəriəd/
Nereid-Voyager2.jpg
4.4357 ± 13≈ 24005504000+360.145.80.74919491949 Kuiper
IX Halimede ‡ /ˌhæləˈmiːdiː/
N2002n1b.jpg
10.0≈ 62≈ 1216590500−1879.78119.60.52120022003 Holman et al.
XI Sao ♦ /ˈseɪoʊ/
Sao VLT-FORS1 2002-09-03 annotated.gif
11.1≈ 44≈ 3.422239900+2919.4350.20.29620022003Holman et al.Sao
S/2002 N 5 ♦
S-2002 N 5 VLT-FORS1 2002-09-03 annotated.gif
11.2≈ 38≈ 323414700+3156.5646.30.43320022024Holman et al.Sao
XII Laomedeia ♦ /ˌleɪəməˈdiːə/
Laomedeia VLT-FORS1 2002-09-03.gif
10.8≈ 42≈ 3.423499900+3176.1336.90.41920022003Holman et al.Sao
X Psamathe ♥ /ˈsæməθiː/
Psamathe arrow.png
11.0≈ 40≈ 2.947615100−9149.51127.80.41420032003 Sheppard et al.Neso
XIII Neso ♥ /ˈniːsoʊ/
Neso VLT-FORS1 2002-09-03.gif
10.7≈ 60≈ 1149895300−9794.99128.40.45520022003Holman et al.Neso
S/2021 N 1 ♥12.1≈ 25≈ 0.850700200−10036.65135.20.50320212024Sheppard et al.Neso

See also

Notes

  1. ↑ The geometric albedo of an astronomical body is the ratio of its actual brightness at zero phase angle (i.e. as seen from the light source) to that of an idealized flat, fully reflecting, diffusively scattering (Lambertian) disk with the same cross-section. The Bond albedo, named after the American astronomer George Phillips Bond (1825–1865), who originally proposed it, is the fraction of power in the total electromagnetic radiation incident on an astronomical body that is scattered back out into space. The Bond albedo is a value strictly between 0 and 1, as it includes all possible scattered light (but not radiation from the body itself). This is in contrast to other definitions of albedo such as the geometric albedo, which can be above 1. In general, though, the Bond albedo may be greater or smaller than the geometric albedo, depending on surface and atmospheric properties of the body in question.
  2. ↑ Binary objects, objects with moons such as the Pluto–Charon system, are quite common among the larger trans-Neptunian objects (TNOs). Around 11% of all TNOs may be binaries. [36]
  3. ↑ Label refers to the Roman numeral attributed to each moon in order of their discovery. [16]
  4. ↑ Diameters with multiple entries such as "60×40×34" reflect that the body is not spherical and that each of its dimensions has been measured well enough to provide a 3-axis estimate. The dimensions of the five inner moons were taken from Karkoschka, 2003. [25] Dimensions of Proteus are from Stooke, 1994. [23] Dimensions of Triton are from Thomas, 2000, [39] whereas its diameter is taken from Davies et al., 1991. [40] The size of Nereid is from Kiss et al., 2016, [32] and the sizes of the other outer moons are from Sheppard, with the diameters of S/2002 N 5 and S/2021 N 1 calculated assuming an albedo of 0.04. [34]
  5. ↑ Of all known moons of Neptune, only Triton has a reliably measured mass. [41] The masses of all regular satellites were estimated by JPL, [41] while all other irregular moons of Neptune were calculated assuming a density of 1 g/cm3.
  6. ↑ Since the reference Showalter et al. (2019) does not cover irregular moons (with colored background), their eccentricities are taken from Planetary Satellite Mean Elements of JPL. [1]

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<span class="mw-page-title-main">Larissa (moon)</span> Moon of Neptune

Larissa, also known as Neptune VII, is the fifth-closest inner satellite of Neptune. It is named after Larissa, a lover of Poseidon.

<span class="mw-page-title-main">Thalassa (moon)</span> Moon of Neptune

Thalassa, also known as Neptune IV, is the second-innermost satellite of Neptune. Thalassa was named after sea goddess Thalassa, a daughter of Aether and Hemera from Greek mythology. "Thalassa" is also the Greek word for "sea".

<span class="mw-page-title-main">Despina (moon)</span> Moon of Neptune

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<span class="mw-page-title-main">Galatea (moon)</span> Moon of Neptune

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<span class="mw-page-title-main">Halimede (moon)</span> Moon of Neptune


Halimede, or Neptune IX, is a retrograde irregular satellite of Neptune. It was discovered by Matthew J. Holman, John J. Kavelaars, Tommy Grav, Wesley C. Fraser and Dan Milisavljevic on August 14, 2002.

<span class="mw-page-title-main">Neso (moon)</span> Outer moon of Neptune

Neso, also known as Neptune XIII, is the second-outermost known natural satellite of Neptune, after S/2021 N 1. It is a retrograde irregular moon discovered by Matthew J. Holman, Brett J. Gladman, et al. on 14 August 2002, though it went unnoticed until 2003. Neso is the second-most distant moon of Neptune, with an average orbital distance of over 49 million km. At its farthest point of its orbit, the satellite is more than 72 million km from Neptune. This distance exceeds Mercury's aphelion, which is approximately 70 million km from the Sun.

<span class="mw-page-title-main">Psamathe (moon)</span> Moon of Neptune

Psamathe, also known as Neptune X, is a retrograde irregular satellite of Neptune. It is named after Psamathe, one of the Nereids. Psamathe was discovered by Scott S. Sheppard and David C. Jewitt in 2003 using the 8.2 meter Subaru telescope. Before it was officially named on February 3, 2007, it was known by the provisional designation S/2003 N 1.

<span class="mw-page-title-main">Moons of Uranus</span> Natural satellites of the planet Uranus

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The rings of Neptune consist primarily of five principal rings. They were first discovered by simultaneous observations of a stellar occultation on 22 July 1984 by André Brahic's and William B. Hubbard's teams at La Silla Observatory (ESO) and at Cerro Tololo Interamerican Observatory in Chile. They were eventually imaged in 1989 by the Voyager 2 spacecraft. At their densest, they are comparable to the less dense portions of Saturn's main rings such as the C ring and the Cassini Division, but much of Neptune's ring system is quite faint and dusty, in some aspects more closely resembling the rings of Jupiter. Neptune's rings are named after astronomers who contributed important work on the planet: Galle, Le Verrier, Lassell, Arago, and Adams. Neptune also has a faint unnamed ring coincident with the orbit of the moon Galatea. Three other moons orbit between the rings: Naiad, Thalassa and Despina.

<span class="mw-page-title-main">Irregular moon</span> Captured satellite following an irregular orbit

In astronomy, an irregular moon, irregular satellite, or irregular natural satellite is a natural satellite following a distant, inclined, and often highly elliptical and retrograde orbit. They have been captured by their parent planet, unlike regular satellites, which formed in orbit around them. Irregular moons have a stable orbit, unlike temporary satellites which often have similarly irregular orbits but will eventually depart. The term does not refer to shape; Triton, for example, is a round moon but is considered irregular due to its orbit and origins.

In astronomy, an inner moon or inner natural satellite is a natural satellite following a prograde, low-inclination orbit inwards of the large satellites of the parent planet. They are generally thought to have been formed in situ at the same time as the coalescence of the original planet. Neptune's moons are an exception, as they are likely reaggregates of the pieces of the original bodies, which were disrupted after the capture of the large moon Triton. Inner satellites are distinguished from other regular satellites by their proximity to the parent planet, their short orbital periods, their low mass, small size, and irregular shapes.

<span class="mw-page-title-main">Exploration of Neptune</span> Overview of the exploration of Neptune

Neptune has been directly explored by one space probe, Voyager 2, in 1989. As of 2024, there are no confirmed future missions to visit the Neptunian system, although a tentative Chinese mission has been planned for launch in 2024. NASA, ESA, and independent academic groups have proposed future scientific missions to visit Neptune. Some mission plans are still active, while others have been abandoned or put on hold.

<span class="mw-page-title-main">Retrograde and prograde motion</span> Relative directions of orbit or rotation

Retrograde motion in astronomy is, in general, orbital or rotational motion of an object in the direction opposite the rotation of its primary, that is, the central object. It may also describe other motions such as precession or nutation of an object's rotational axis. Prograde or direct motion is more normal motion in the same direction as the primary rotates. However, "retrograde" and "prograde" can also refer to an object other than the primary if so described. The direction of rotation is determined by an inertial frame of reference, such as distant fixed stars.

<span class="mw-page-title-main">Hippocamp (moon)</span> Smallest moon of Neptune

Hippocamp, also designated Neptune XIV, is a small moon of Neptune discovered on 1 July 2013. It was found by astronomer Mark Showalter by analyzing archived Neptune photographs the Hubble Space Telescope captured between 2004 and 2009. The moon is so dim that it was not observed when the Voyager 2 space probe flew by Neptune and its moons in 1989. It is about 35 km (20 mi) in diameter, and orbits Neptune in about 23 hours, just under one Earth day. Due to its unusually close distance to Neptune's largest inner moon Proteus, it has been hypothesized that Hippocamp may have accreted from material ejected by an impact on Proteus several billion years ago. The moon was formerly known by its provisional designation S/2004 N 1 until February 2019, when it was formally named Hippocamp, after the mythological sea-horse symbolizing Poseidon in Greek mythology.

The following outline is provided as an overview of and topical guide to Neptune:

<span class="mw-page-title-main">S/2002 N 5</span> Outer moon of Neptune

S/2002 N 5 is a prograde irregular satellite of Neptune. It was discovered on 14 August 2002 by Matthew Holman, John J. Kavelaars, Tommy Grav, and Wesley Fraser using the 4.0-meter Víctor M. Blanco Telescope at Cerro Tololo Observatory, Chile, but it became lost and was not observed again until Scott S. Sheppard rediscovered it on 3 September 2021. The discovery of S/2002 N 5 was announced on 23 February 2024, after observations were collected over a long enough time to confirm the satellite's orbit. S/2002 N 5 orbits Neptune at an average distance of over 23 million km (14 million mi) and takes almost 9 Earth years to complete its orbit.

References

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