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Moons of Neptune

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The planet Neptune has 16 known moons, which are named for minor water deities and a water creature in Greek mythology.[note 1] By far the largest of them is Triton, discovered by William Lassell on 10 October 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.

Shown in this image are Neptune and some of its moons: Triton, Galatea, Naiad, Thalassa, Despina, Proteus, and Larissa
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.

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

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Discovery

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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 24 May 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
  Moons of Neptune

Names

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See also: Name conflicts with minor planets

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 equivalent of 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

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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
 
Size comparison of Neptune's seven inner moons

Regular moons

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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

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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

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Main article: Triton (moon)
 
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 2] 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

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Main article: Nereid (moon)

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

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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

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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

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 3] 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

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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 (7) ♠ Triton (1) † Nereid (1)
‡ Halimede (1) ♦ Sao group (3) ♥ Neso group (3)
Neptunian moons
Label
[note 4] 		Name Pronunciation
(key) 		Image Abs.
magn. 		Diameter
(km)
[note 5] 		Mass
(×1016 kg)
[note 6] 		Semi-major axis
(km)
[17] 		Orbital period
(d)
[1] 		Orbital inclination
(°)
[1] 		Eccentricity
[17][note 7] 		Discovery
year
[16] 		Year announced Discoverer
[16] 		Group
III Naiad /ˈneɪəd, ˈnaɪæd/[42]
 
 9.6 60.4
(96 × 60 × 52)		 ≈ 13 48224 +0.2944 4.691 0.0047 1989 1989 Voyager Science Team inner
IV Thalassa /θəˈlæsə/
 
 8.7 81.4
(108 × 100 × 52)		 ≈ 35 50074 +0.3115 0.135 0.0018 1989 1989 Voyager Science Team inner
V Despina /dəˈspaɪnə/
 
 7.3 156
(180 × 148 × 128)		 ≈ 170 52526 +0.3346 0.068 0.0004 1989 1989 Voyager Science Team inner
VI Galatea /ˌɡæləˈtiːə/
 
 7.2 174.8
(204 × 184 × 144)		 ≈ 280 61953 +0.4287 0.034 0.0001 1989 1989 Voyager Science Team inner
VII Larissa /ləˈrɪsə/
 
 6.8 194
(216 × 204 × 168)		 ≈ 380 73548 +0.5555 0.205 0.0012 1981 1981 Reitsema et al. inner
XIV Hippocamp /ˈhɪpəkæmp/
 
 10.5 34.8±4.0 ≈ 2.2 105283 +0.9500 0.064 0.0005 2013 2013 Showalter et al. inner
VIII Proteus /ˈproʊtiəs/
 
 5.0 420
(436 × 416 × 402)		 ≈ 3900 117646 +1.1223 0.075 0.0005 1989 1989 Voyager Science Team inner
I Triton♠ /ˈtraɪtən/
 
 –1.2 2705.2±4.8
(2709 × 2706 × 2705)		 2139000 354759 −5.8769 156.865 0.0000 1846 1846 Lassell
II Nereid† /ˈnɪəriəd/
 
 4.4 357 ± 13 ≈ 2400 5513900 +360.13 5.1 0.751 1949 1949 Kuiper
IX Halimede‡ /ˌhæləˈmiːdiː/
 
 10.0 ≈ 62 ≈ 12 16590500 −1879 119.6 0.521 2002 2003 Holman et al.
XI Sao♦ /ˈseɪoʊ/
 
 11.1 ≈ 44 ≈ 3.4 22239900 +2919 50.2 0.296 2002 2003 Holman et al. Sao
S/2002 N 5♦
 
 11.2 ≈ 38 ≈ 3 23414700 +3151 46.3 0.433 2002 2024 Holman et al. Sao
XII Laomedeia♦ /ˌleɪəməˈdiːə/
 
 10.8 ≈ 42 ≈ 3.4 23499900 +3168 36.9 0.419 2002 2003 Holman et al. Sao
X Psamathe♥ /ˈsæməθiː/
 
 11.0 ≈ 40 ≈ 2.9 47646600 −9149 127.8 0.413 2003 2003 Sheppard et al. Neso
XIII Neso♥ /ˈniːsoʊ/
 
 10.7 ≈ 60 ≈ 11 49897800 −9805 128.4 0.455 2002 2003 Holman et al. Neso
S/2021 N 1♥ 12.1 ≈ 25 ≈ 0.8 50700200 −10043 135.2 0.503 2021 2024 Sheppard et al. Neso

See also

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Notes

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  1. ^ This is a IAU guideline that will be followed at the naming of every Neptunian moon, although two (S/2002 N 5 and S/2021 N 1) have yet to receive permanent names.
  2. ^ 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.
  3. ^ 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]
  4. ^ Label refers to the Roman numeral attributed to each moon in order of their discovery.
    [16]
  5. ^ 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]
  6. ^ 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.
  7. ^ 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]

References

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  1. ^ a b c d e "Planetary Satellite Mean Elements". Jet Propulsion Laboratory. Archived from the original on 9 October 2024. Retrieved 9 October 2024. Note: Orbital elements of regular satellites are with respect to the Laplace plane, while orbital elements of irregular satellites are with respect to the ecliptic. Inclinations greater than 90° are retrograde. Orbital periods of irregular satellites may not be consistent with their semi-major axes due to perturbations.
  2. ^ a b "MPEC 2024-D112 : S/2021 N 1". Minor Planet Electronic Circular. Minor Planet Center. 23 February 2024. Archived from the original on 5 March 2024. Retrieved 23 February 2024.
  3. ^ Lassell, W. (1846). "Discovery of supposed ring and satellite of Neptune". Monthly Notices of the Royal Astronomical Society. 7: 157. Bibcode:1846MNRAS...7..157L. doi:10.1093/mnras/7.9.154.
  4. ^ Kuiper, Gerard P. (1949). "The Second Satellite of Neptune". Publications of the Astronomical Society of the Pacific. 61 (361): 175–176. Bibcode:1949PASP...61..175K. doi:10.1086/126166.
  5. ^ Reitsema, Harold J.; Hubbard, William B.; Lebofsky, Larry A.; Tholen, David J. (1982). "Occultation by a Possible Third Satellite of Neptune". Science. 215 (4530): 289–291. Bibcode:1982Sci...215..289R. doi:10.1126/science.215.4530.289. PMID 17784355. S2CID 21385195.
  6. ^ a b c d e f g h i j k Smith, B. A.; Soderblom, L. A.; Banfield, D.; Barnet, C.; Basilevsky, A. T.; Beebe, R. F.; Bollinger, K.; Boyce, J. M.; Brahic, A. (1989). "Voyager 2 at Neptune: Imaging Science Results". Science. 246 (4936): 1422–1449. Bibcode:1989Sci...246.1422S. doi:10.1126/science.246.4936.1422. PMID 17755997. S2CID 45403579. Archived from the original on 2020-08-04. Retrieved 2019-06-25.
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  10. ^ Showalter, M. R. (2013-07-15). "How to Photograph a Racehorse ...and how this relates to a tiny moon of Neptune". Mark Showalter's blog. Archived from the original on 2013-07-18. Retrieved 2013-07-16.
  11. ^ Kelly Beatty (15 July 2013). "Neptune's Newest Moon". Sky & Telescope. Archived from the original on 16 July 2013. Retrieved 12 June 2017.
  12. ^ a b "New Uranus and Neptune Moons". Earth & Planetary Laboratory. Carnegie Institution for Science. 23 February 2024. Archived from the original on 23 February 2024. Retrieved 23 February 2024.
  13. ^ "MPEC 2024-D114 : S/2002 N 5". Minor Planet Electronic Circular. Minor Planet Center. 23 February 2024. Archived from the original on 3 March 2024. Retrieved 23 February 2024.
  14. ^ Flammarion, Camille (1880). Astronomie populaire (in French). Flammarion. p. 591. ISBN 2-08-011041-1. Archived from the original on 2012-03-01. Retrieved 2009-03-04.
  15. ^ Moore, Patrick (April 1996). The planet Neptune: an historical survey before Voyager. Wiley-Praxis Series in Astronomy and Astrophysics (2nd ed.). John Wiley & Sons. pp. 150 (see p. 68). ISBN 978-0-471-96015-7. OCLC 33103787.
  16. ^ a b c d e "Planet and Satellite Names and Discoverers". Gazetteer of Planetary Nomenclature. USGS Astrogeology. Archived from the original on 2010-07-03. Retrieved 2022-06-23.
  17. ^ a b c Showalter, M. R.; de Pater, I.; Lissauer, J. J.; French, R. S. (2019). "The seventh inner moon of Neptune" (PDF). Nature. 566 (7744): 350–353. Bibcode:2019Natur.566..350S. doi:10.1038/s41586-019-0909-9. PMC 6424524. PMID 30787452. Archived (PDF) from the original on 2019-02-22. Retrieved 2019-02-22.
  18. ^ M. Antonietta Barucci; Hermann Boehnhardt; Dale P. Cruikshank; Alessandro Morbidelli, eds. (2008). "Irregular Satellites of the Giant Planets" (PDF). The Solar System Beyond Neptune. University of Arizona Press. p. 414. ISBN 9780816527557. Archived from the original (PDF) on 2017-08-10. Retrieved 2017-07-22.
  19. ^ a b c d Jewitt, David; Haghighipour, Nader (2007). "Irregular Satellites of the Planets: Products of Capture in the Early Solar System" (PDF). Annual Review of Astronomy and Astrophysics. 45 (1): 261–95. arXiv:astro-ph/0703059. Bibcode:2007ARA&A..45..261J. doi:10.1146/annurev.astro.44.051905.092459. S2CID 13282788. Archived (PDF) from the original on 2014-02-25. Retrieved 2010-09-27.
  20. ^ Williams, David R. (1 September 2004). "Neptune Fact Sheet". NASA. Archived from the original on 1 July 2010. Retrieved 18 July 2013.
  21. ^ a b c d Miner, Ellis D.; Wessen, Randii R.; Cuzzi, Jeffrey N. (2007). "Present knowledge of the Neptune ring system". Planetary Ring System. Springer Praxis Books. ISBN 978-0-387-34177-4.
  22. ^ Horn, Linda J.; Hui, John; Lane, Arthur L.; Colwell, Joshua E. (1990). "Observations of Neptunian rings by Voyager photopolarimeter experiment". Geophysical Research Letters. 17 (10): 1745–1748. Bibcode:1990GeoRL..17.1745H. doi:10.1029/GL017i010p01745.
  23. ^ a b c Stooke, Philip J. (1994). "The surfaces of Larissa and Proteus". Earth, Moon, and Planets. 65 (1): 31–54. Bibcode:1994EM&P...65...31S. doi:10.1007/BF00572198. S2CID 121825800.
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