Wikipedia

Neptune

eighth and farthest planet from the Sun in the Solar System

This article is about the planet. For the Roman God of the Sea, see Neptune (mythology).

Neptune is the eighth and farthest planet from the Sun in the Solar System. It is an ice giant. It is the fourth-largest planet in the system.

Neptune ♆, historically also ⯉
Neptune in true color[a] as captured by Voyager 2. Like Uranus, Neptune has a muted appearance; several storms can still be seen, such as the Great Dark Spot at the center.
Discovery[1]
Discovered by
Discovery date23 September 1846
Designations
PronunciationUS: /ˈnɛptuːn/ (audio speaker iconlisten), UK: /-tjuːn/[2]
Named after
Latin Neptunus, via French Neptune
AdjectivesNeptunian (/nɛpˈtjuːniən/),[3] Poseidean[4]
Orbital characteristics[9][b]
Epoch J2000
Aphelion30.33 AU (4.54 billion km)
Perihelion29.81 AU (4.46 billion km)
30.07 AU (4.50 billion km)
Eccentricity0.008678
367.49 days[6]
5.43 km/s[6]
259.883°
Inclination1.770° to ecliptic
6.43° to Sun's equator
0.74° to invariable plane[7]
131.783°
2042-Sep-04[8]
273.187°
Known satellites16
Physical characteristics
Mean radius
24,622±19 km[10][c]
Equatorial radius
24,764±15 km[10][c]
3.883 Earths
Polar radius
24,341±30 km[10][c]
3.829 Earths
Flattening0.0171±0.0013
7.6187×109 km2[11][c]
14.98 Earths
Volume6.253×1013 km3[6][c]
57.74 Earths
Mass1.02413×1026 kg[6]
17.147 Earths
5.15×10−5 Suns
Mean density
1.638 g/cm3[6][d]
11.15 m/s2[6][c]
1.14 g
0.23[12] (estimate)
23.5 km/s[6][c]
0.67125 d
16 h 6 m 36 s[5]
0.6713 day[6]
16 h 6 min 36 s
Equatorial rotation velocity
2.68 km/s (9,650 km/h)
28.32° (to orbit)[6]
North pole right ascension
 19h 57m 20s[10]
299.3°
North pole declination
42.950°[10]
Albedo0.290 (bond)[13]
0.442 (geom.)[14]
Surface temp. min mean max
1 bar level 72 K (−201 °C)[6]
0.1 bar (10 kPa) 55 K (−218 °C)[6]
7.67[15] to 8.00[15]
−6.9[16]
2.2–2.4″[6][17]
Atmosphere[6]
19.7±0.6 km
Composition by volume
  • 80%±3.2% hydrogen
  • 19%±3.2% helium
  • 1.5%±0.5% methane
  • ~0.019% hydrogen deuteride
  • ~0.00015% ethane
  • Icy volatiles:

Neptune's mass is 17 times Earth's mass and a little bit more than Uranus' mass. Neptune is denser and smaller than Uranus. Because of its greater mass, Neptune's gravity makes its atmosphere smaller and denser.

It was named after the Roman god of the sea, Neptune. Neptune's astronomical symbol is ♆, the trident of the god Neptune.

Neptune's atmosphere is mostly hydrogen and helium. It also contains small amounts of methane which makes the planet appear blue.[18][19][20] Neptune's blue color is similar, but slightly darker, than the color of Uranus. Neptune also has the strongest winds of any planet in the Solar System, as high as 2,100 km/h or 1,300 mph. [21]

Urbain Le Verrier and John Couch Adams were the astronomers who discovered Neptune. Neptune was not discovered using a telescope. It was the first planet to be discovered using mathematics. In 1821, astronomers saw that Uranus' orbit was different from what they expected. Another nearby planet's mass was changing Uranus' orbit. They found Neptune was the cause.

Voyager 2 visited Neptune on 25 August 1989. It was the only spacecraft to visit the planet. Neptune used to have a huge storm known as the "Great Dark Spot". Voyager 2 discovered the spot in 1989. The dark spot was not seen in 1994, but new spots were found since then. It is not known why the dark spot disappeared. Visits by other space probes have been planned.

Neptune has five rings surrounding it. However, the rings are hard to see from Earth.

History

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Galileo Galilei
 
Urbain Le Verrier, the co-discoverer of Neptune

Discovery

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Galileo Galilei was the first person to see Neptune.[22] He saw it on 28 December 1612 and 27 January 1613.[22] His drawings showed the points where Neptune is placed, it is near Jupiter.[22] But Galileo was not credited for the discovery. He thought Neptune was a "fixed star" instead of a planet. Because Neptune moved slowly across the sky, Galileo's small telescope was not strong enough to see that Neptune was a planet.[23]

In 1821, Alexis Bouvard published the astronomical tables of the orbit of Uranus.[24][25] Later observations showed that Uranus was orbiting in an irregular way.[26] Some astronomers thought this was caused by another large planet.[26] In 1843, John Couch Adams calculated the orbit of an eighth planet that could possibly affect the orbit of Uranus. He sent his calculations to Sir George Airy, the Astronomer Royal. George Airy asked Adams for an explanation.[27] In 1846, Urbain Le Verrier made his own calculations but also failed to get much attention from French astronomers.[25][28] Airy saw his calculations and encouraged James Challis to search for the planet. Challis began his search in July 1846. Meanwhile, Le Verrier had convinced Johann Gottfried Galle to search for the planet.[28]

Heinrich d'Arrest, a student at the Berlin Observatory, suggested that a newly drawn map of the sky in the region of Le Verrier's predicted area could be compared with the current sky.[28] This map was needed to look for the change of position of a planet, compared to a fixed star. Neptune was discovered the same night on 23 September 1846.[29] It was found 1° from where Le Verrier had thought it would be. It was about 1.5° from Adams' prediction.[30] Challis later found out that he had seen the planet twice in August. He did not recognize it at the time because of his careless work approach.[28] Neptune became the first planet to be discovered by mathematical calculations instead of a telescope.[31]

 
Neptune (red line) completes its orbit every 164 years

Crediting and naming

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When Neptune was discovered, the French and the British could not agree on who would get credit for the discovery. Later, an international agreement decided that both Le Verrier and Adams deserved credit. However, historians reviewed the topic after the rediscovery in 1998 of the "Neptune papers" (historical documents from the Royal Greenwich Observatory). It had seemingly been stolen by astronomer Olin Eggen for almost 30 years. It was only found again (in his ownership) shortly after his death.[32] After looking at the documents, some historians now think that Adams does not deserve equal credit with Le Verrier.[33]

Shortly after its discovery, Neptune was temporarily called "the planet exterior to Uranus" or "Le Verrier's planet". The first suggestion for a name came from Galle. He proposed the name Janus. In England, Challis suggested the name Oceanus.[34] In France, Arago suggested that the new planet be called Leverrier, but a lot of people outside France disagreed with this. French almanacs quickly reintroduced the name Herschel for Uranus and Leverrier for Neptune.[27]

Meanwhile, Adams suggested changing the name Georgian to Uranus, while Le Verrier (through the Board of Longitude) suggested Neptune for the new planet. Struve supported the name Neptune on 29 December 1846, to the Saint Petersburg Academy of Sciences.[35] Soon, Neptune was internationally agreed as the official name for the new planet. In Roman mythology, Neptune was the god of the sea, identified with the Greek god, Poseidon.[36][37][38] Neptune's astrological symbol is Neptune's trident (♆).[39]

Structure

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Mass and composition

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Neptune's mass is between that of the Earth and the largest gas giants.[40] Neptune is the fourth largest planet in the Solar System and the third most massive.[31] Neptune is 17 times the mass of Earth, but just ​1⁄18 the mass of Jupiter.[41] Neptune is a little bit more massive than Uranus, though Neptune is denser and smaller in size than Uranus.[31] Neptune and Uranus are often considered a part of "ice giants" (a sub-class of gas giants).[31][42] They are smaller in size than Jupiter and Saturn, and have different compositions. To search extrasolar planets, Neptune has been used as a reference to compare the size and structure of other discovered planets. Some discovered planets that have similar masses like Neptune are often called "Neptunes".[43]

The atmosphere of Neptune is made up mostly of hydrogen, with a smaller amount of helium. A tiny amount of methane was also detected in the atmosphere. The methane gives Neptune its blue color.[44][45] The color of Neptune is similar, but slightly darker, than the color of Uranus.[45]

Because of Neptune's far distance from the Sun, it gets very little heat. The average surface temperature on Neptune is about −201°C (−331 °F; 72 K).[46] Therefore, at its surface Neptune is the coldest planet in the Solar System.

But in the depths of the planet, the temperature rises. The source of this heating is unclear.[47][48][49] Neptune is the farthest planet from the Sun,[31] yet its internal energy is strong enough to create the fastest winds seen in the Solar System, at 1,300 miles per hour (2,100 km/h).[50][51] Several possible explanations have been suggested. Firstly, radiogenic heating from the planet's core. Among the explanations is the continued radiation into space of leftover heat made by infalling matter during the planet's birth. Another explanation is gravity waves breaking above the tropopause. It has also been suggested that the friction and ram pressure of the diamond hail heats up the planet.[52][53]

The structure inside Neptune is thought to be similar to the structure inside Uranus.[54] There is likely to be a core, thought to be about 1.5 Earth masses.[55] It is made up of molten rock and metal surrounded by rock, water, ammonia, and methane.[55] This mixture is referred to as icy. It is called a water-ammonia ocean.[56] More mixtures of methane, ammonia, and water are found in the lower areas of the atmosphere.[54] At a depth of 7,000 km of Neptune, the methane may decomposes into diamond crystals. These diamond crystals look like hailstones.[57][58]

Neptune
 
Comparison of the size of Neptune and Earth
 
Internal structure of Neptune
 
The Great Dark Spot as seen from Voyager 2

Weather and magnetic field

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One difference between Neptune and Uranus is the level of its meteorological activity. When the Voyager spacecraft flew by Uranus in 1986, the winds on that planet were observed not so strong as on Neptune. When Voyager flew by Neptune in 1989, powerful weather events were observed.[59] The weather of Neptune has very active storms.[51] Its atmosphere has the highest wind speeds in the Solar System. It may be powered by internal heat flow. Regular winds in the equatorial region have speeds of around 1,200 km/h (750 mph). Winds in storm systems can reach up to 2,100 km/h, near-supersonic speeds.[60]

In 1989, the Great Dark Spot, an anticyclonic storm system, was discovered by NASA's Voyager 2 spacecraft.[61][62] On 2 November 1994, the Hubble Space Telescope did not see the Great Dark Spot on the planet. Instead, a new storm similar to the Great Dark Spot was found in the planet's northern hemisphere.[63] The reason why the Great Dark Spot has disappeared is unknown.[64] The Scooter is another storm, a white cloud group farther south than the Great Dark Spot.[65] Its nickname was given when first noticed in the months leading up to the Voyager encounter in 1989.[65] It moved faster than the Great Dark Spot.[66] Later images showed clouds that moved even faster than Scooter. The Wizard's Eye/Dark Spot 2 is another southern cyclonic storm, the second strongest storm seen during the 1989 encounter. It originally was completely dark, but as Voyager came closer to the planet, a bright core developed.[67]

 
Neptune cloud cover over three decades (1994–2020)[68]

In August 2023, the clouds vanished. The possible reason is solar flare.[68] 30 years of Neptune' weather observations by Hubble Space Telescope showed that cloud activity is related to solar cycles.[69]

Neptune also has similarities with Uranus in its magnetosphere. However, Uranus' magnetosphere is weaker than Neptune's magnetosphere.[42][70] The magnetic field is strongly tilted compared to its rotational axis at 47°. It is offset at least 0.55 radii (about 13,500 kilometres, bigger than the Earth's diameter, for scale) from the planet's physical center. The unusual course may be caused by flows in the interior of the planet.[70]

Neptune has a similar axial tilt to Earth, so it will have seasons. Its seasons last about 40 years.[71]

Neptune's rings

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See the main article: Rings of Neptune
 
Neptune's rings and moons viewed by the James Webb Space Telescope

There are five rings around the planet.[31] They are not as well known as the rings of Saturn. The rings were discovered by a team led by an American scientist Edward Guinan in 1968. Then, in the mid-1980s astronomers thought that the rings might not be complete. Stellar occultations were found that rarely showed an extra "blink" just before or after the planet moved in front of the star. However, Voyager 2 showed that they were complete. The planetary rings of Neptune have a weird "clumpy" arrangement. Scientists think that it may be because of the gravitational contact with small moons that orbit near them.[72] Pictures showed that the ring system had several faint rings. The farthest ring, Adams, has five arcs named Courage, Liberté, Egalité 1, Egalité 2, and Fraternité (Courage, Liberty, Equality, and Fraternity).[73]

 
Neptune's rings

The laws of motion predict that arcs will spread out into one ring in a very short time. But the arcs in Neptune's rings somehow did not. A moon's gravity may have created the arcs. Galatea is a moon just inside the Adams ring.[74] However, in 2005, scientists figured out that Neptune's rings were more unstable than previously believed. The Liberté arc may disappear in roughly less than 100 years.[75]

Neptune's moons

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See the main article: List of Neptune's moons

Neptune has 16 known moons.[76] As Neptune was the Roman god of the sea, the planet's moons were named after lesser sea gods or goddesses.[77]

The largest moon of Neptune is Triton. Triton was discovered on 10 October 1846 by British astronomer William Lassell.[78] Unlike all other large planetary moons, Triton orbits in the other direction to the other moons.[79] This shows the moon was probably captured.[79] It is close enough to Neptune to be locked into a synchronous orbit. It is also slowly moving into Neptune and may one day be torn apart when it passes the Roche limit.[80] Triton is the coldest object that has been measured in the Solar System, with temperatures of −235 °C (38 K, −392 °F).[81]

Neptune's second known moon (by order of discovery), the odd moon Nereid, has one of the most unusual orbits of any satellite in the Solar System.[82] Nereid is so far from Neptune that it requires 360 Earth days to make one orbit.[82] It causes the largest elliptical orbit and the largest deviation from a circular path.[82]

Some of these moons have been speculated to have been possible Kupier belt objects, which in turn became a part of Neptune's orbit.

From July to September 1989, Voyager 2 discovered six new moons of Neptune.[83] Of these, Proteus is the second most massive Neptunian moon.[84] It has only one quarter of 1% of the mass of Triton.[84] Neptune's closest four moons, Naiad, Thalassa, Despina, and Galatea, orbit close enough to be inside Neptune's rings. The next farthest out, Larissa was discovered in 1981 when it had covered up light from a star.[85] The moon was credited for causing Neptune's ring arcs when Voyager 2 observed Neptune in 1989. Five new unusual moons discovered between 2002 and 2003 were announced in 2004.[86][87] The latest moon, Hippocamp, was discovered from examining Hubble Telescope images on 16 July 2013.[88]

 
Neptune and Triton in true sizes and distances from each other
A 15-hour time-lapse of Neptune in the near-infrared captured by Hubble. Triton is clearly visible, while others appear much smaller.
Moons
 
Neptune (top) and Triton (bottom)
 
A Voyager 2 mosaic of Triton
 
Proteus

Observation

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Neptune cannot be seen by just looking at the sky with the naked eye. To see it, a telescope or binoculars is needed.[89] This is because Neptune has a normal brightness between magnitudes +7.7 and +8.0.[89] It can be outshined by Jupiter's Galilean moons, the dwarf planet Ceres, and the asteroids 4 Vesta, 2 Pallas, 7 Iris, 3 Juno and 6 Hebe.[90] A telescope or strong binoculars show Neptune as a small blue dot that looks similar to Uranus. The blue color comes from the methane in its atmosphere.[91] Its small size in the night sky has made it difficult to study visually. Most telescopic data was quite limited until the arrival of the Hubble Space Telescope and large ground-based telescopes with adaptive optics.[92]

The average distance between Neptune and the Sun is about 4.5 billion km.[31] Therefore, Neptune completes its orbit once every 164 years. On 12 July 2011, Neptune completed its first orbit since its discovery in 1846.[93]

Exploration

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See the main article: Exploration of Neptune
 
Voyager 2

Currently, only one spacecraft has visited Neptune. NASA's Voyager 2 probe made a quick fly-by of the planet with its closest encounter on 25 August 1989.[94][95]

One of Voyager 2's important discoveries was its very close fly-by of Triton, where it took pictures of several parts of the moon.[96] The pictures were sent back to Earth from Voyager 2 in 1989. The probe also discovered the Great Dark Spot. However, it had now disappeared after the Hubble Space Telescope took pictures of Neptune in 1994. Originally thought to be a large cloud or cyclonic storm system.[97] It was later guessed to be a hole in the visible cloud deck.[98]

Proposed missions

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  • Interstellar Express—Two probes by CNSA to explore the heliosphere. The second probe would come within 1,000 km of Neptune in 2038.[99]
  • ODINUS—This mission uses two spacecraft to study the Neptunian and Uranian systems. 2034 is the launch date.[100][101]
  • OSS mission—This is a mission by ESA and NASA. Its focus is to map the gravitational fields in deep space, including the Outer Solar System (up to 50 AU).[102]
  • Triton Hopper—A NIAC plan for a mission to Neptune to land on Neptune's moon Triton and then fly to several places.[103]
  • Trident—This is a finalist in the Discovery Program. It will fly close to Neptune once in 2038 and closely study its largest moon Triton.[104]
  • Neptune Odyssey—An idea for a NASA mission to observe Neptune's atmosphere and the weather, and its moon Triton. It would launch in 2033 and arrive at Neptune in 2049.[105]

References

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  1. ↑ Hamilton, Calvin J. (4 August 2001). "Neptune". Views of the Solar System. Archived from the original on 15 July 2007. Retrieved 13 August 2007.
  2. ↑ Walter, Elizabeth (21 April 2003). Cambridge Advanced Learner's Dictionary (2nd ed.). Cambridge University Press. ISBN 978-0-521-53106-1.
  3. ↑ "Neptunian". Oxford English Dictionary. Oxford University Press. 2nd ed. 1989.
  4. ↑ "Enabling Exploration with Small Radioisotope Power Systems" (PDF). NASA. September 2004. Archived from the original (PDF) on 22 December 2016. Retrieved 26 January 2016.
  5. ↑ 5.0 5.1 Seligman, Courtney. "Rotation Period and Day Length". Archived from the original on 28 July 2011. Retrieved 13 August 2009.
  6. ↑ 6.00 6.01 6.02 6.03 6.04 6.05 6.06 6.07 6.08 6.09 6.10 6.11 6.12 Williams, David R. (1 September 2004). "Neptune Fact Sheet". NASA. Archived from the original on 1 July 2010. Retrieved 14 August 2007.
  7. ↑ Souami, D.; Souchay, J. (July 2012). "The solar system's invariable plane". Astronomy & Astrophysics. 543: 11. Bibcode:2012A&A...543A.133S. doi:10.1051/0004-6361/201219011. ISSN 0004-6361. A133.
  8. ↑ "HORIZONS Planet-center Batch call for September 2042 Perihelion". ssd.jpl.nasa.gov (Perihelion for Neptune's planet-center (899) occurs on 2042-Sep-04 at 29.80647406au during a rdot flip from negative to positive). NASA/JPL. Archived from the original on 7 September 2021. Retrieved 2021-09-07.
  9. ↑ Yeomans, Donald K. "HORIZONS Web-Interface for Neptune Barycenter (Major Body=8)". JPL Horizons On-Line Ephemeris System. Archived from the original on 7 September 2021. Retrieved 18 July 2014.—Select "Ephemeris Type: Orbital Elements", "Time Span: 2000-01-01 12:00 to 2000-01-02". ("_target Body: Neptune Barycenter" and "Center: Solar System Barycenter (@0)".)
  10. ↑ 10.0 10.1 10.2 10.3 10.4 Cite error: The named reference Seidelmann Archinal A'hearn et al. 2007 was used but no text was provided for refs named (see the help page).
  11. ↑ Cite error: The named reference fact2 was used but no text was provided for refs named (see the help page).
  12. ↑ de Pater, Imke; Lissauer, Jack J. (2015). Planetary Sciences (2nd updated ed.). New York: Cambridge University Press. p. 250. ISBN 978-0-521-85371-2. Archived from the original on 26 November 2016. Retrieved 17 August 2016.
  13. ↑ Cite error: The named reference Pearl_et_al_Neptune was used but no text was provided for refs named (see the help page).
  14. ↑ Cite error: The named reference Mallama_et_al was used but no text was provided for refs named (see the help page).
  15. ↑ 15.0 15.1 Cite error: The named reference Mallama_and_Hilton was used but no text was provided for refs named (see the help page).
  16. ↑ "Encyclopedia - the brightest bodies". IMCCE. Archived from the original on 24 July 2023. Retrieved 2023-05-29.
  17. ↑ Espenak, Fred (20 July 2005). "Twelve Year Planetary Ephemeris: 1995–2006". NASA. Archived from the original on 5 December 2012. Retrieved 1 March 2008.
  18. ↑ info@noirlab.edu. "Gemini North Telescope helps explain why Uranus and Neptune are different colors - observations from Gemini Observatory, a program of NSF's NOIRLab, and other telescopes reveal that excess haze on Uranus makes it paler than Neptune". www.noirlab.edu. Retrieved 2022-07-30.
  19. ↑ Laboratory, By NSF’s NOIRLab (National Optical-Infrared Astronomy Research. "Why Uranus and Neptune Are Different Colors". NASA Solar System Exploration. Retrieved 2023-03-06.
  20. ↑ Magazine, Smithsonian; Kuta, Sarah. "Why Neptune Appears Bluer Than Its Cousin Uranus". Smithsonian Magazine. Retrieved 2022-07-30.
  21. ↑ Suomi, V.E.; Limaye, S.S.; Johnson, D.R. (1991). "High Winds of Neptune: A possible mechanism". Science. 251 (4996): 929–32. Bibcode:1991Sci...251..929S. doi:10.1126/science.251.4996.929. PMID 17847386. S2CID 46419483.
  22. ↑ 22.0 22.1 22.2 Hirschfeld, Alan (2001). Parallax:The Race to Measure the Cosmos. New York, New York: Henry Holt. ISBN 0-8050-7133-4.
  23. ↑ Littmann, Mark; Standish, E.M. (2004). Planets Beyond: Discovering the Outer Solar System. Courier Dover Publications. ISBN 978-0-486-43602-9.{{cite book}}: CS1 maint: location missing publisher (link)
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  25. ↑ 25.0 25.1 "Neptune: The first planet discovered by mathematical rather than observational means: discovered simultaneously by Le Verrier and Adams : History of Information". Jeremy Norman's History of Information. Retrieved 2021-06-14.
  26. ↑ 26.0 26.1 [Anon.] (2001) "Bouvard, Alexis", Encyclopædia Britannica, Deluxe CDROM edition
  27. ↑ 27.0 27.1 "John Couch Adams' account of the discovery of Neptune". Maths History. Retrieved 10 May 2021.
  28. ↑ 28.0 28.1 28.2 28.3 Airy, G. B. (1 January 1970). "Account of some circumstances historically connected with the discovery of the planet exterior to Uranus". Astronomische Nachrichten No. 585. 25 (10): 131–148. doi:10.1002/asna.18470251002.
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  30. ↑ Chambers, John; Mitton, Jacqueline (2014). From dust to life: the origin and evolution of our solar system. Princeton, New Jersey: Princeton University Press. pp. 38–39. ISBN 978-0-691-14522-8. OCLC 859181634.
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  40. ↑ At 102.413×1024kg,"Neptune Fact Sheet". nssdc.gsfc.nasa.gov. Retrieved 2021-06-14.
  41. ↑ Bradford A. Smith, «Neptune », 'World Book Online Reference Center', 2004, p. 5
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  47. ↑ Broadfoot A.L.; Atreya S.K.; Bertaux J.L.; et al. 1999. Ultraviolet Spectrometer Observations of Neptune and Triton. Science. 246 (4936): 1459–66. Bibcode:1989Sci...246.1459B. doi:10.1126/science.246.4936.1459. PMID 17756000. S2CID 21809358. Archived (PDF) from the original on 28 May 2008. Retrieved 12 March 2008.
  48. ↑ Herbert, Floyd; Sandel, Bill R. August/September 1999. Ultraviolet observations of Uranus and Neptune. Planetary and Space Science 47 (8–9): 1, 119–139. Bibcode:1999P&SS...47.1119H. doi:10.1016/S0032-0633(98)00142-1
  49. ↑ Elkins-Tanton, Linda T. (2006). Uranus, Neptune, Pluto, and the Outer Solar System. Infobase Publishing. p. 75. ISBN 978-1-4381-0729-5.
  50. ↑ Suomi, V. E.; Limaye, S. S.; Johnson, D. R. (1991). "High winds of Neptune - A possible mechanism". Science. 251 (4996): 929–932. Bibcode:1991Sci...251..929S. doi:10.1126/science.251.4996.929. PMID 17847386. S2CID 46419483.
  51. ↑ 51.0 51.1 Cain, Fraser (2008-12-09). "What is the Weather Like on Neptune?". Universe Today. Retrieved 2021-06-12.
  52. ↑ McHugh J.P. Computation of gravity waves near the tropopause Archived 27 October 2007 at the Wayback Machine, AAS/Division for Planetary Sciences Meeting Abstracts, p. 53.07, September 1999
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  1. ↑ Based on Irwin, Patrick G J; Dobinson, Jack; James, Arjuna; Teanby, Nicholas A; Simon, Amy A; Fletcher, Leigh N; Roman, Michael T; Orton, Glenn S; Wong, Michael H; Toledo, Daniel; Pérez-Hoyos, Santiago; Beck, Julie (2023-12-23). "Modelling the seasonal cycle of Uranus's colour and magnitude, and comparison with Neptune". Monthly Notices of the Royal Astronomical Society. 527 (4): 11521–11538. doi:10.1093/mnras/stad3761. ISSN 0035-8711.
  2. ↑ Orbital elements refer to the Neptune barycentre and Solar System barycentre. These are the instantaneous osculating values at the precise J2000 epoch. Barycentre quantities are given because, in contrast to the planetary centre, they do not experience appreciable changes on a day-to-day basis from the motion of the moons.
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 Refers to the level of 1 bar (100 kPa) atmospheric pressure
  4. ↑ Based on the volume within the level of 1 bar atmospheric pressure

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