Template:About Template:Use British English Template:Use dmy dates Template:Pp-move-indefTemplate:Pp-semi-indef

Diameter km
Distance from primary km
Mass Template:Val/delimitnum/gaps00×1026Template:Val/units[1]
17.147 Earths
5.15×10-5 Suns
Density Template:Val/delimitnum/gaps00Template:Val/units[1][lower-alpha 1]

Neptune is the eighth and farthest planet from the Sun in the Solar System. It is the fourth-largest planet by diameter and the third-largest by mass. Among the gaseous planets in the Solar System, Neptune is the most dense. Neptune is 17 times the mass of Earth and is slightly more massive than its near-twin Uranus, which is 15 times the mass of Earth but not as dense.[lower-alpha 2] Neptune orbits the Sun at an average distance of 30.1 astronomical units. Named after the Roman god of the sea, its astronomical symbol is ♆, a stylised version of the god Neptune's trident.

Neptune was the first planet found by mathematical prediction rather than by empirical observation. Unexpected changes in the orbit of Uranus led Alexis Bouvard to deduce that its orbit was subject to gravitational perturbation by an unknown planet. Neptune was subsequently observed on 23 September 1846[2] by Johann Galle within a degree of the position predicted by Urbain Le Verrier, and its largest moon, Triton, was discovered shortly thereafter, though none of the planet's remaining 13 moons were located telescopically until the 20th century. Neptune has been visited by one spacecraft, Voyager 2, which flew by the planet on 25 August 1989.[3]

Neptune is similar in composition to Uranus, and both have compositions which differ from those of the larger gas giants, Jupiter, and Saturn. Neptune's atmosphere, although similar to Jupiter's and Saturn's in that it is composed primarily of hydrogen and helium, along with traces of hydrocarbons and possibly nitrogen, contains a higher proportion of "ices" such as water, ammonia, and methane. Astronomers sometimes categorise Uranus and Neptune as "ice giants" to emphasise these distinctions.[4] The interior of Neptune, like that of Uranus, is primarily composed of ices and rock.[5] Perhaps the core has a solid surface, but the temperature would be thousands of degrees and the atmospheric pressure crushing.[6] Traces of methane in the outermost regions in part account for the planet's blue appearance.[7]

In contrast to the hazy, relatively featureless atmosphere of Uranus, Neptune's atmosphere is notable for its active and visible weather patterns. For example, at the time of the 1989 Voyager 2 flyby, the planet's southern hemisphere possessed a Great Dark Spot comparable to the Great Red Spot on Jupiter. These weather patterns are driven by the strongest sustained winds of any planet in the Solar System, with recorded wind speeds as high as 2,100 kilometres per hour (1,300 mph).[8] Because of its great distance from the Sun, Neptune's outer atmosphere is one of the coldest places in the Solar System, with temperatures at its cloud tops approaching 55 K (−218 °C). Temperatures at the planet's centre are approximately 5,400 K (5,000 °C).[9][10] Neptune has a faint and fragmented ring system (labelled "arcs"), which may have been detected during the 1960s but was only indisputably confirmed in 1989 by Voyager 2.[11]



Main article: Discovery of Neptune

Some of the earliest recorded observations ever made through a telescope, Galileo's drawings on 28 December 1612 and 27 January 1613, contain plotted points that match up with what is now known to be the position of Neptune. On both occasions, Galileo seems to have mistaken Neptune for a fixed star when it appeared close—in conjunction—to Jupiter in the night sky;[12] hence, he is not credited with Neptune's discovery. During the period of his first observation in December 1612, Neptune was stationary in the sky because it had just turned retrograde that day. This apparent backward motion is created when Earth's orbit takes it past an outer planet. Because Neptune was only beginning its yearly retrograde cycle, the motion of the planet was far too slight to be detected with Galileo's small telescope.[13] In July 2009, University of Melbourne physicist David Jamieson announced new evidence suggesting that Galileo was at least aware that the star he had observed had moved relative to the fixed stars.[14]

In 1821, Alexis Bouvard published astronomical tables of the orbit of Neptune's neighbour Uranus.[15] Subsequent observations revealed substantial deviations from the tables, leading Bouvard to hypothesize that an unknown body was perturbing the orbit through gravitational interaction.[16] In 1843, John Couch Adams began work on the orbit of Uranus using the data he had. Via Cambridge Observatory director James Challis, he requested extra data from Sir George Airy, the Astronomer Royal, who supplied it in February 1844. Adams continued to work in 1845–46 and produced several different estimates of a new planet.[17][18]

File:Urbain Le Verrier.jpg

In 1845–46, Urbain Le Verrier, independently of Adams, developed his own calculations but also experienced difficulties in stimulating any enthusiasm in his compatriots. In June 1846, upon seeing Le Verrier's first published estimate of the planet's longitude and its similarity to Adams's estimate, Airy persuaded Challis to search for the planet. Challis vainly scoured the sky throughout August and September.[16][19]

Meantime, Le Verrier by letter urged Berlin Observatory astronomer Johann Gottfried Galle to search with the observatory's refractor. Heinrich d'Arrest, a student at the observatory, suggested to Galle that they could compare a recently drawn chart of the sky in the region of Le Verrier's predicted location with the current sky to seek the displacement characteristic of a planet, as opposed to a fixed star. The evening of the day of receipt of Le Verrier's letter on 23 September 1846, Neptune was discovered within 1° of where Le Verrier had predicted it to be, and about 12° from Adams' prediction. Challis later realised that he had observed the planet twice in August (Neptune had been observed on 8 and 12 August, but because Challis lacked an up-to-date star-map it was not recognised as a planet), failing to identify it owing to his casual approach to the work.[16][20]

In the wake of the discovery, there was much nationalistic rivalry between the French and the British over who had priority and deserved credit for the discovery. Eventually an international consensus emerged that both Le Verrier and Adams jointly deserved credit. Since 1966 Dennis Rawlins has questioned the credibility of Adams's claim to co-discovery and the issue was re-evaluated by historians with the return in 1998 of the "Neptune papers" (historical documents) to the Royal Observatory, Greenwich.[21] After reviewing the documents, they suggest that "Adams does not deserve equal credit with Le Verrier for the discovery of Neptune. That credit belongs only to the person who succeeded both in predicting the planet's place and in convincing astronomers to search for it."[22]


Shortly after its discovery, Neptune was referred to simply as "the planet exterior to Uranus" or as "Le Verrier's planet". The first suggestion for a name came from Galle, who proposed the name Janus. In England, Challis put forward the name Oceanus.[23]

Claiming the right to name his discovery, Le Verrier quickly proposed the name Neptune for this new planet, though falsely stating that this had been officially approved by the French Bureau des Longitudes.[24] In October, he sought to name the planet Le Verrier, after himself, and he had loyal support in this from the observatory director, François Arago. This suggestion met with stiff resistance outside France.[25] French almanacs quickly reintroduced the name Herschel for Uranus, after that planet's discoverer Sir William Herschel, and Leverrier for the new planet.[26]

Struve came out in favour of the name Neptune on 29 December 1846, to the Saint Petersburg Academy of Sciences.[27] Soon Neptune became the internationally accepted name. In Roman mythology, Neptune was the god of the sea, identified with the Greek Poseidon. The demand for a mythological name seemed to be in keeping with the nomenclature of the other planets, all of which, except for Earth, were named for deities in Greek and Roman mythology.[28]

Most languages today, even in countries that have no direct link to Greco-Roman culture, use some variant of the name "Neptune" for the planet; in Chinese, Japanese and Korean, the planet's name was literally translated as "sea king star" (Template:Lang), because Neptune was the god of the sea.[29] In modern Greek, though, the planet is called Poseidon (Ποσειδώνας: Poseidonas), the Greek counterpart to Neptune.[30]


From its discovery in 1846 until the subsequent discovery of Pluto in 1930, Neptune was the farthest known planet. Upon Pluto's discovery Neptune became the penultimate planet, save for a 20-year period between 1979 and 1999 when Pluto's elliptical orbit brought it closer to the Sun than Neptune.[31] The discovery of the Kuiper belt in 1992 led many astronomers to debate whether Pluto should be considered a planet in its own right or part of the belt's larger structure.[32][33] In 2006, the International Astronomical Union defined the word "planet" for the first time, reclassifying Pluto as a "dwarf planet" and making Neptune once again the last planet in the Solar System.[34]

Composition and structureEdit

File:Neptune, Earth size comparison.jpg

With a mass of 1.0243×1026 kg,[1] Neptune is an intermediate body between Earth and the larger gas giants: its mass is 17 times that of Earth but just 1/19th that of Jupiter.[lower-alpha 2] Its surface gravity is surpassed only by Jupiter.[35] Neptune's equatorial radius of 24,764 km[36] is nearly four times that of Earth. Neptune and Uranus are often considered a subclass of gas giant termed "ice giants", due to their smaller size and higher concentrations of volatiles relative to Jupiter and Saturn.[37] In the search for extrasolar planets Neptune has been used as a metonym: discovered bodies of similar mass are often referred to as "Neptunes",[38] just as astronomers refer to various extra-solar bodies as "Jupiters".

Internal structureEdit

Neptune's internal structure resembles that of Uranus. Its atmosphere forms about 5% to 10% of its mass and extends perhaps 10% to 20% of the way towards the core, where it reaches pressures of about 10 GPa, or about 100,000 times that of Earth's atmosphere. Increasing concentrations of methane, ammonia and water are found in the lower regions of the atmosphere.[9]

File:Neptune diagram.svg

The mantle is equivalent to 10 to 15 Earth masses and is rich in water, ammonia and methane.[2] As is customary in planetary science, this mixture is referred to as icy even though it is a hot, highly dense fluid. This fluid, which has a high electrical conductivity, is sometimes called a water–ammonia ocean.[39] The mantle may consist of a layer of ionic water where the water molecules break down into a soup of hydrogen and oxygen ions, and deeper down superionic water in which the oxygen crystallises but the hydrogen ions float around freely within the oxygen lattice.[40] At a depth of 7000 km, the conditions may be such that methane decomposes into diamond crystals that rain downwards like hailstones.[41] Very-high-pressure experiments at the Lawrence Livermore National Laboratory suggest that the base of the mantle may comprise an ocean of liquid diamond, with floating solid 'diamond-bergs'.[42][43]

The core of Neptune is composed of iron, nickel and silicates, with an interior model giving a mass about 1.2 times that of Earth.[44] The pressure at the centre is 7 Mbar (700 GPa), about twice as high as that at the centre of Earth, and the temperature may be 5,400 K.[9][10]



At high altitudes, Neptune's atmosphere is 80% hydrogen and 19% helium.[9] A trace amount of methane is also present. Prominent absorption bands of methane occur at wavelengths above 600 nm, in the red and infrared portion of the spectrum. As with Uranus, this absorption of red light by the atmospheric methane is part of what gives Neptune its blue hue,[45] although Neptune's vivid azure differs from Uranus's milder cyan. Because Neptune's atmospheric methane content is similar to that of Uranus, some unknown atmospheric constituent is thought to contribute to Neptune's colour.[7]

Neptune's atmosphere is subdivided into two main regions; the lower troposphere, where temperature decreases with altitude, and the stratosphere, where temperature increases with altitude. The boundary between the two, the tropopause, occurs at a pressure of 0.1 bars (10 kPa).[4] The stratosphere then gives way to the thermosphere at a pressure lower than 10−5 to 10−4 microbars (1 to 10 Pa).[4] The thermosphere gradually transitions to the exosphere.

File:Neptune clouds.jpg

Models suggest that Neptune's troposphere is banded by clouds of varying compositions depending on altitude. The upper-level clouds occur at pressures below one bar, where the temperature is suitable for methane to condense. For pressures between one and five bars (100 and 500 kPa), clouds of ammonia and hydrogen sulfide are believed to form. Above a pressure of five bars, the clouds may consist of ammonia, ammonium sulfide, hydrogen sulfide and water. Deeper clouds of water ice should be found at pressures of about 50 bars (5.0 MPa), where the temperature reaches 273 K (0 °C). Underneath, clouds of ammonia and hydrogen sulfide may be found.[46]

High-altitude clouds on Neptune have been observed casting shadows on the opaque cloud deck below. There are also high-altitude cloud bands that wrap around the planet at constant latitude. These circumferential bands have widths of 50–150 km and lie about 50–110 km above the cloud deck.[47] These altitudes are in the layer where weather occurs, the troposphere. Weather does not occur in the higher stratosphere or thermosphere. Unlike Uranus, Neptune's composition has a higher volume of ocean, whereas Uranus has a smaller mantle.[48]

Neptune's spectra suggest that its lower stratosphere is hazy due to condensation of products of ultraviolet photolysis of methane, such as ethane and acetylene.[4][9] The stratosphere is also home to trace amounts of carbon monoxide and hydrogen cyanide.[4][49] The stratosphere of Neptune is warmer than that of Uranus due to the elevated concentration of hydrocarbons.[4]

For reasons that remain obscure, the planet's thermosphere is at an anomalously high temperature of about 750 K.[50][51] The planet is too far from the Sun for this heat to be generated by ultraviolet radiation. One candidate for a heating mechanism is atmospheric interaction with ions in the planet's magnetic field. Other candidates are gravity waves from the interior that dissipate in the atmosphere. The thermosphere contains traces of carbon dioxide and water, which may have been deposited from external sources such as meteorites and dust.[46][49]


Neptune also resembles Uranus in its magnetosphere, with a magnetic field strongly tilted relative to its rotational axis at 47° and offset at least 0.55 radii, or about 13500 km from the planet's physical centre. Before Voyager 2's arrival at Neptune, it was hypothesised that Uranus's tilted magnetosphere was the result of its sideways rotation. In comparing the magnetic fields of the two planets, scientists now think the extreme orientation may be characteristic of flows in the planets' interiors. This field may be generated by convective fluid motions in a thin spherical shell of electrically conducting liquids (probably a combination of ammonia, methane and water)[46] resulting in a dynamo action.[52]

The dipole component of the magnetic field at the magnetic equator of Neptune is about 14 microteslas (0.14 G).[53] The dipole magnetic moment of Neptune is about 2.2Template:Esp T·m3 (14 μT·RN3, where RN is the radius of Neptune). Neptune's magnetic field has a complex geometry that includes relatively large contributions from non-dipolar components, including a strong quadrupole moment that may exceed the dipole moment in strength. By contrast, Earth, Jupiter and Saturn have only relatively small quadrupole moments, and their fields are less tilted from the polar axis. The large quadrupole moment of Neptune may be the result of offset from the planet's centre and geometrical constraints of the field's dynamo generator.[54][55]

Neptune's bow shock, where the magnetosphere begins to slow the solar wind, occurs at a distance of 34.9 times the radius of the planet. The magnetopause, where the pressure of the magnetosphere counterbalances the solar wind, lies at a distance of 23–26.5 times the radius of Neptune. The tail of the magnetosphere extends out to at least 72 times the radius of Neptune, and likely much farther.[54]

Planetary ringsEdit

Main article: Rings of Neptune

Neptune has a planetary ring system, though one much less substantial than that of Saturn. The rings may consist of ice particles coated with silicates or carbon-based material, which most likely gives them a reddish hue.[56] The three main rings are the narrow Adams Ring, 63,000 km from the centre of Neptune, the Le Verrier Ring, at 53,000 km, and the broader, fainter Galle Ring, at 42,000 km. A faint outward extension to the Le Verrier Ring has been named Lassell; it is bounded at its outer edge by the Arago Ring at 57,000 km.[57]

The first of these planetary rings was discovered in 1968 by a team led by Edward Guinan,[11][58] but it was later thought that this ring might be incomplete.[59] Evidence that the rings might have gaps first arose during a stellar occultation in 1984 when the rings obscured a star on immersion but not on emersion.[60] Images by Voyager 2 in 1989 settled the issue by showing several faint rings. These rings have a clumpy structure,[61] the cause of which is not understood but which may be due to the gravitational interaction with small moons in orbit near them.[62]

The outermost ring, Adams, contains five prominent arcs now named Courage, Liberté, Egalité 1, Egalité 2 and Fraternité (Courage, Liberty, Equality and Fraternity).[63] The existence of arcs was difficult to explain because the laws of motion would predict that arcs would spread out into a uniform ring over short timescales. Astronomers now believe that the arcs are corralled into their current form by the gravitational effects of Galatea, a moon just inward from the ring.[64][65]

Earth-based observations announced in 2005 appeared to show that Neptune's rings are much more unstable than previously thought. Images taken from the W. M. Keck Observatory in 2002 and 2003 show considerable decay in the rings when compared to images by Voyager 2. In particular, it seems that the Liberté arc might disappear in as little as one century.[66]


One difference between Neptune and Uranus is the typical level of meteorological activity. When the Voyager 2 spacecraft flew by Uranus in 1986, that planet was visually quite bland. In contrast Neptune exhibited notable weather phenomena during the 1989 Voyager 2 fly-by.[67]

File:Neptune storms.jpg

Neptune's weather is characterised by extremely dynamic storm systems, with winds reaching speeds of almost 600 m/s (1340 mph)—nearly attaining supersonic flow.[8] More typically, by tracking the motion of persistent clouds, wind speeds have been shown to vary from 20 m/s in the easterly direction to 325 m/s westward.[69] At the cloud tops, the prevailing winds range in speed from 400 m/s along the equator to 250 m/s at the poles.[46] Most of the winds on Neptune move in a direction opposite the planet's rotation.[70] The general pattern of winds showed prograde rotation at high latitudes vs. retrograde rotation at lower latitudes. The difference in flow direction is believed to be a "skin effect" and not due to any deeper atmospheric processes.[4] At 70° S latitude, a high-speed jet travels at a speed of 300 m/s.[4]

The abundance of methane, ethane and ethyne at Neptune's equator is 10–100 times greater than at the poles. This is interpreted as evidence for upwelling at the equator and subsidence near the poles.[4]Template:Clarify

In 2007, it was discovered that the upper troposphere of Neptune's south pole was about 10 K warmer than the rest of Neptune, which averages approximately 73 K (−200 °C).[71] The warmth differential is enough to let methane, which elsewhere lies frozen in Neptune's upper atmosphere, leak out as gas through the south pole and into space. The relative "hot spot" is due to Neptune's axial tilt, which has exposed the south pole to the Sun for the last quarter of Neptune's year, or roughly 40 Earth years. As Neptune slowly moves towards the opposite side of the Sun, the south pole will be darkened and the north pole illuminated, causing the methane release to shift to the north pole.[72]

Because of seasonal changes, the cloud bands in the southern hemisphere of Neptune have been observed to increase in size and albedo. This trend was first seen in 1980 and is expected to last until about 2020. The long orbital period of Neptune results in seasons lasting forty years.[73]


Neptune's Great Dark Spot

The Great Dark Spot, as imaged by Voyager 2

In 1989, the Great Dark Spot, an anti-cyclonic storm system spanning 13000×6600 km,[67] was discovered by NASA's Voyager 2 spacecraft. The storm resembled the Great Red Spot of Jupiter. Some five years later, 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.[74]

The Scooter is another storm, a white cloud group farther south than the Great Dark Spot. Its nickname came when it was first detected in the months before the 1989 Voyager 2 encounter it moved faster than the Great Dark Spot.[70] Subsequent images revealed even faster clouds. The Small Dark Spot is a southern cyclonic storm, the second-most-intense storm observed during the 1989 encounter. It initially was completely dark, but as Voyager 2 approached the planet, a bright core developed and can be seen in most of the highest-resolution images.[75]

Neptune's dark spots are thought to occur in the troposphere at lower altitudes than the brighter cloud features,[76] so they appear as holes in the upper cloud decks. As they are stable features that can persist for several months, they are thought to be vortex structures.[47] Often associated with dark spots are brighter, persistent methane clouds that form around the tropopause layer.[77] The persistence of companion clouds shows that some former dark spots may continue to exist as cyclones even though they are no longer visible as a dark feature. Dark spots may dissipate when they migrate too close to the equator or possibly through some other unknown mechanism.[78]

Internal heatingEdit

File:Different Faces Neptune.jpg

Neptune's more varied weather when compared to Uranus is believed to be due in part to its higher internal heating. Although Neptune lies half again as far from the Sun as Uranus, and receives only 40% its amount of sunlight,[4] the two planets' surface temperatures are roughly equal.[80] The upper regions of Neptune's troposphere reach a low temperature of 51.8 K (−221.3 °C). At a depth where the atmospheric pressure equals 1 bar (100 kPa), the temperature is 72.00 K (−201.15 °C).[81] Deeper inside the layers of gas, the temperature rises steadily. As with Uranus, the source of this heating is unknown, but the discrepancy is larger: Uranus only radiates 1.1 times as much energy as it receives from the Sun;[82] whereas Neptune radiates about 2.61 times as much energy as it receives from the Sun.[83] Neptune is the farthest planet from the Sun, yet its internal energy is sufficient to drive the fastest planetary winds seen in the Solar System. Depending on the thermal properties of its interior, the heat left over from Neptune's formation may be sufficient to explain its current heat flow, though it is more difficult to simultaneously explain Uranus's lack of internal heat while preserving the apparent similarity between the two planets.[84]

Orbit and rotationEdit

File:Neptune Orbit.gif

The average distance between Neptune and the Sun is 4.50 billion km (about 30.1 AU), and it completes an orbit on average every 164.79 years, subject to a variability of around ±0.1 years. The perihelion distance is 29.81 AU; the aphelion distance is 30.33 AU.[85]

On 11 July 2011, Neptune completed its first full barycentric orbit since its discovery in 1846,[86][87] although it did not appear at its exact discovery position in the sky, because Earth was in a different location in its 365.26-day orbit. Because of the motion of the Sun in relation to the barycentre of the Solar System, on 11 July Neptune was also not at its exact discovery position in relation to the Sun; if the more common heliocentric coordinate system is used, the discovery longitude was reached on 12 July 2011.[88][89][90]

The elliptical orbit of Neptune is inclined 1.77° compared to that of Earth.

The axial tilt of Neptune is 28.32°,[91] which is similar to the tilts of Earth (23°) and Mars (25°). As a result, this planet experiences similar seasonal changes. The long orbital period of Neptune means that the seasons last for forty Earth years.[73] Its sidereal rotation period (day) is roughly 16.11 hours.[88] Because its axial tilt is comparable to Earth's, the variation in the length of its day over the course of its long year is not any more extreme.

Because Neptune is not a solid body, its atmosphere undergoes differential rotation. The wide equatorial zone rotates with a period of about 18 hours, which is slower than the 16.1-hour rotation of the planet's magnetic field. By contrast, the reverse is true for the polar regions where the rotation period is 12 hours. This differential rotation is the most pronounced of any planet in the Solar System,[92] and it results in strong latitudinal wind shear.[47]

Orbital resonancesEdit

File:TheKuiperBelt classes-en.svg

Neptune's orbit has a profound impact on the region directly beyond it, known as the Kuiper belt. The Kuiper belt is a ring of small icy worlds, similar to the asteroid belt but far larger, extending from Neptune's orbit at 30 AU out to about 55 AU from the Sun.[93] Much in the same way that Jupiter's gravity dominates the asteroid belt, shaping its structure, so Neptune's gravity dominates the Kuiper belt. Over the age of the Solar System, certain regions of the Kuiper belt became destabilised by Neptune's gravity, creating gaps in the Kuiper belt's structure. The region between 40 and 42 AU is an example.[94]

There do exist orbits within these empty regions where objects can survive for the age of the Solar System. These resonances occur when Neptune's orbital period is a precise fraction of that of the object, such as 1:2, or 3:4. If, say, an object orbits the Sun once for every two Neptune orbits, it will only complete half an orbit by the time Neptune returns to its original position. The most heavily populated resonance in the Kuiper belt, with over 200 known objects,[95] is the 2:3 resonance. Objects in this resonance complete 2 orbits for every 3 of Neptune, and are known as plutinos because the largest of the known Kuiper belt objects, Pluto, is among them.[96] Although Pluto crosses Neptune's orbit regularly, the 2:3 resonance ensures they can never collide.[97] The 3:4, 3:5, 4:7 and 2:5 resonances are less populated.[98]

Neptune possesses a number of trojan objects occupying the Sun-Neptune Template:L4 Lagrangian point—a gravitationally stable region leading it in its orbit.[99] Neptune trojans can be viewed as being in a 1:1 resonance with Neptune. Some Neptune trojans are remarkably stable in their orbits, and are likely to have formed alongside Neptune rather than being captured. The first and so far only object identified as associated with Neptune's trailing Template:L5 Lagrangian point is 2008 LC18.[100] Neptune also has a temporary quasi-satellite, Template:Mpl.[101] The object has been a quasi-satellite of Neptune for about 12,500 years and it will remain in that dynamical state for another 12,500 years. It is likely a captured object.[101]

Formation and migrationEdit


The formation of the ice giants, Neptune and Uranus, has proven difficult to model precisely. Current models suggest that the matter density in the outer regions of the Solar System was too low to account for the formation of such large bodies from the traditionally accepted method of core accretion, and various hypotheses have been advanced to explain their creation. One is that the ice giants were not created by core accretion but from instabilities within the original protoplanetary disc and later had their atmospheres blasted away by radiation from a nearby massive OB star.[37]

An alternative concept is that they formed closer to the Sun, where the matter density was higher, and then subsequently migrated to their current orbits after the removal of the gaseous protoplanetary disc.[102] This hypothesis of migration after formation is favoured, due to its ability to better explain the occupancy of the populations of small objects observed in the trans-Neptunian region.[103] The current most widely accepted[104][105][106] explanation of the details of this hypothesis is known as the Nice model, which explores the effect of a migrating Neptune and the other giant planets on the structure of the Kuiper belt.


Main article: Moons of Neptune
For a timeline of discovery dates, see Timeline of discovery of Solar System planets and their moons.

Neptune has 14 known moons.[1][107] The largest by far, comprising more than 99.5% of the mass in orbit around Neptune[lower-alpha 3] and the only one massive enough to be spheroidal, is Triton, discovered by William Lassell just 17 days after the discovery of Neptune itself. Unlike all other large planetary moons in the Solar System, Triton has a retrograde orbit, indicating that it was captured rather than forming in place; it was probably once a dwarf planet in the Kuiper belt.[108] It is close enough to Neptune to be locked into a synchronous rotation, and it is slowly spiralling inward because of tidal acceleration. It will eventually be torn apart, in about 3.6 billion years, when it reaches the Roche limit.[109] In 1989, Triton was the coldest object that had yet been measured in the solar system,[110] with estimated temperatures of 38 K (−235 °C).[111]

Neptune's second known satellite (by order of discovery), the irregular moon Nereid, has one of the most eccentric orbits of any satellite in the solar system. The eccentricity of 0.7512 gives it an apoapsis that is seven times its periapsis distance from Neptune.[lower-alpha 4]

File:Proteus (Voyager 2).jpg

From July to September 1989, Voyager 2 discovered six new Neptunian moons.[54] Of these, the irregularly shaped Proteus is notable for being as large as a body of its density can be without being pulled into a spherical shape by its own gravity.[112] Although the second-most-massive Neptunian moon, it is only 0.25% the mass of Triton. Neptune's innermost four moons—Naiad, Thalassa, Despina and Galatea—orbit close enough to be within Neptune's rings. The next-farthest out, Larissa, was originally discovered in 1981 when it had occulted a star. This occultation had been attributed to ring arcs, but when Voyager 2 observed Neptune in 1989, it was found to have caused it. Five new irregular moons discovered between 2002 and 2003 were announced in 2004.[113][114] A new moon and the smallest yet, S/2004 N 1, was found in 2013. Because Neptune was the Roman god of the sea, Neptune's moons have been named after lesser sea gods.[28]


Neptune is never visible to the naked eye, having a brightness between magnitudes +7.7 and +8.0,[1][115] which can be outshone by Jupiter's Galilean moons, the dwarf planet Ceres and the asteroids 4 Vesta, 2 Pallas, 7 Iris, 3 Juno and 6 Hebe.[116] A telescope or strong binoculars will resolve Neptune as a small blue disk, similar in appearance to Uranus.[117]

Because of the distance of Neptune from Earth, the angular diameter of the planet only ranges from 2.2 to 2.4 arcseconds,[1][115] the smallest of the Solar System planets. Its small apparent size has made it challenging to study visually. Most telescopic data was fairly limited until the advent of Hubble Space Telescope and large ground-based telescopes with adaptive optics.[118][119]

From Earth, Neptune goes through apparent retrograde motion every 367 days, resulting in a looping motion against the background stars during each opposition. These loops carried it close to the 1846 discovery coordinates in April and July 2010 and again in October and November 2011.[90]

Observation of Neptune in the radio-frequency band shows that the planet is a source of both continuous emission and irregular bursts. Both sources are believed to originate from the planet's rotating magnetic field.[46] In the infrared part of the spectrum, Neptune's storms appear bright against the cooler background, allowing the size and shape of these features to be readily tracked.[120]


File:Triton moon mosaic Voyager 2 (large).jpg

Voyager 2's closest approach to Neptune occurred on 25 August 1989. Because this was the last major planet the spacecraft could visit, it was decided to make a close flyby of the moon Triton, regardless of the consequences to the trajectory, similarly to what was done for Voyager 1's encounter with Saturn and its moon Titan. The images relayed back to Earth from Voyager 2 became the basis of a 1989 PBS all-night program, Neptune All Night.[121]

During the encounter, signals from the spacecraft required 246 minutes to reach Earth. Hence, for the most part, the Voyager 2 mission relied on preloaded commands for the Neptune encounter. The spacecraft performed a near-encounter with the moon Nereid before it came within 4400 km of Neptune's atmosphere on 25 August, then passed close to the planet's largest moon Triton later the same day.[122]

The spacecraft verified the existence of a magnetic field surrounding the planet and discovered that the field was offset from the centre and tilted in a manner similar to the field around Uranus. The question of the planet's rotation period was settled using measurements of radio emissions. Voyager 2 also showed that Neptune had a surprisingly active weather system. Six new moons were discovered, and the planet was shown to have more than one ring.[54][122]

In 2003, there was a proposal in NASA's "Vision Missions Studies" for a "Neptune Orbiter with Probes" mission that does Cassini-level science. The work is being done in conjunction with JPL and the California Institute of Technology.[123] Another, more recent proposal was for Argo, a flyby spacecraft that would visit Jupiter, Saturn, Neptune, and a Kuiper belt object.[124] However, the focus would be on Neptune and its largest moon Triton to help plug a predicted 50-year gap in exploration of the system.[124][124] New Horizons 2 might have also done a flyby.

See alsoEdit

Template:Portal Template:Wikipedia books


  1. Cite error: Invalid <ref> tag; no text was provided for refs named 1bar
  2. 2.0 2.1 The mass of Earth is 5.9736×1024 kg, giving a mass ratio of:
    \begin{smallmatrix}\frac{M_{Neptune}}{M_{Earth}} \ =\ \frac{1.02 \times 10^{26}}{5.97 \times 10^{24}} \ =\ 17.09\end{smallmatrix}
    The mass of Uranus is 8.6810×1025 kg, giving a mass ratio of:
    \begin{smallmatrix}\frac{M_{Uranus}}{M_{Earth}} \ =\ \frac{8.68 \times 10^{25}}{5.97 \times 10^{24}}\ =\ 14.54\end{smallmatrix}
    The mass of Jupiter is 1.8986×1027 kg, giving a mass ratio of:
    \begin{smallmatrix}\frac{M_{Jupiter}}{M_{Neptune}} \ =\ \frac{1.90 \times 10^{27}}{1.02 \times 10^{26}}\ =\ 18.63\end{smallmatrix}
    Mass values from Williams, David R. (29 November 2007). Planetary Fact Sheet – Metric. NASA. Retrieved 13 March 2008.
  3. Mass of Triton: 2.14×1022 kg. Combined mass of 12 other known moons of Neptune: 7.53×1019 kg, or 0.35%. The mass of the rings is negligible.
  4. \begin{smallmatrix}\frac{r_{a}}{r_{p}} = \frac{2}{1-e}-1 = 2/0.2488-1=7.039.\end{smallmatrix}


  1. Cite error: Invalid <ref> tag; no text was provided for refs named fact
  2. Cite error: Invalid <ref> tag; no text was provided for refs named Hamilton
  3. Template:Cite news
  4. 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 4.8 4.9 Template:Cite doi
  5. Template:Cite doi
  6. Upper Surface of Neptune. (2008-12-09). Retrieved on 2013-07-28.
  7. 7.0 7.1 Munsell, Kirk (13 November 2007). Neptune overview. Solar System Exploration. NASA. Retrieved 20 February 2008.
  8. 8.0 8.1 Suomi, V. E. (1991). High Winds of Neptune: A possible mechanism. Science 251 (4996): 929–932.
  9. 9.0 9.1 9.2 9.3 9.4 Hubbard, W. B. (1997). Neptune's Deep Chemistry. Science 275 (5304): 1279–1280.
  10. 10.0 10.1 Nettelmann, N.. Interior Models of Jupiter, Saturn and Neptune (PDF). University of Rostock. Retrieved 25 February 2008.
  11. 11.0 11.1 Template:Cite news
  12. Hirschfeld, Alan (2001). Parallax: The Race to Measure the Cosmos. New York, New York: Henry Holt. ISBN 978-0-8050-7133-7. 
  13. Littmann, Mark (2004). Planets Beyond: Discovering the Outer Solar System. Courier Dover Publications. ISBN 978-0-486-43602-9. 
  14. Britt, Robert Roy (2009). Galileo discovered Neptune, new theory claims. MSNBC News. Retrieved 10 July 2009.
  15. Bouvard, A. (1821). Tables astronomiques publiées par le Bureau des Longitudes de France. Paris: Bachelier. 
  16. 16.0 16.1 16.2 Airy, G. B. (13 November 1846). Account of some circumstances historically connected with the discovery of the planet exterior to Uranus. Monthly Notices of the Royal Astronomical Society 7: 121–144.
  17. O'Connor, John J. (2006). John Couch Adams' account of the discovery of Neptune. University of St Andrews. Retrieved 18 February 2008.
  18. Adams, J. C. (13 November 1846). Explanation of the observed irregularities in the motion of Uranus, on the hypothesis of disturbance by a more distant planet. Monthly Notices of the Royal Astronomical Society 7.
  19. Challis, Rev. J. (13 November 1846). Account of observations at the Cambridge observatory for detecting the planet exterior to Uranus. Monthly Notices of the Royal Astronomical Society 7: 145–149.
  20. Galle, J. G. (13 November 1846). Account of the discovery of the planet of Le Verrier at Berlin. Monthly Notices of the Royal Astronomical Society 7.
  21. Kollerstrom, Nick (2001). Neptune's Discovery. The British Case for Co-Prediction.. University College London. Archived from the original on 11 November 2005. Retrieved 19 March 2007.
  22. William Sheehan, Nicholas Kollerstrom, Craig B. Waff (December 2004). The Case of the Pilfered Planet – Did the British steal Neptune?.
  23. Moore (2000):206
  24. Littmann, Mark (2004). Planets Beyond, Exploring the Outer Solar System. Courier Dover Publications. ISBN 978-0-486-43602-9. 
  25. Baum, Richard (2003). In Search of Planet Vulcan: The Ghost in Newton's Clockwork Universe. Basic Books, 109–110. ISBN 978-0-7382-0889-3. 
  26. Gingerich, Owen (1958). The Naming of Uranus and Neptune. Astronomical Society of the Pacific Leaflets 8: 9–15.
  27. Hind, J. R. (1847). Second report of proceedings in the Cambridge Observatory relating to the new Planet (Neptune). Astronomische Nachrichten 25 (21).
  28. 28.0 28.1 Blue, Jennifer (17 December 2008). Planet and Satellite Names and Discoverers. USGS. Retrieved 18 February 2008.
  29. Planetary linguistics. Retrieved 8 April 2010.
  30. Greek Names of the Planets. Retrieved 2012-07-14. See also the Greek article about the planet.
  31. Template:Cite news
  32. Weissman, Paul R. (1995). The Kuiper Belt. Annual Review of Astronomy and Astrophysics 33.
  33. The Status of Pluto:A clarification. International Astronomical Union, Press release (1999). Archived from the original on 15 June 2006. Retrieved 25 May 2006.
  34. Template:Cite news
  35. (2001) The New Cosmos: An Introduction to Astronomy and Astrophysics, 5th, Springer. ISBN 978-3-540-67877-9.  See Table 3.1.
  36. Template:Cite doi
  37. 37.0 37.1 Boss, Alan P. (2002). Formation of gas and ice giant planets. Earth and Planetary Science Letters 202 (3–4): 513–523.
  38. Template:Cite news
  39. Atreya, S. (2006). Water-ammonia ionic ocean on Uranus and Neptune?. Geophysical Research Abstracts 8.
  40. Weird water lurking inside giant planets, New Scientist,1 September 2010, Magazine issue 2776.
  41. Kerr, Richard A. (1999). Neptune May Crush Methane Into Diamonds. Science 286 (5437).
  42. Bland, Eric (January 15, 2010). Diamond Oceans Possible on Uranus, Neptune. Retrieved May 17, 2013.
  43. Baldwin, Emily (January 21, 2010). Oceans of diamond possible on Uranus and Neptune. Retrieved February 6, 2014.
  44. Podolak, M. (1995). Comparative models of Uranus and Neptune. Planetary and Space Science 43 (12): 1517–1522.
  45. Crisp, D. (14 June 1995). Hubble Space Telescope Observations of Neptune. Hubble News Center. Retrieved 22 April 2007.
  46. 46.0 46.1 46.2 46.3 46.4 Elkins-Tanton, Linda T. (2006). Uranus, Neptune, Pluto, and the Outer Solar System. New York: Chelsea House, 79–83. ISBN 978-0-8160-5197-7. 
  47. 47.0 47.1 47.2 (2003) Cloud Structures on Neptune Observed with Keck Telescope Adaptive Optics. The Astronomical Journal, 125 (1): 364–375.
  48. Frances, Peter (2008). DK Universe. DK Publishing, 196–201. ISBN 978-0-7566-3670-8. 
  49. 49.0 49.1 Template:Cite doi
  50. Broadfoot, A.L. (1999). Ultraviolet Spectrometer Observations of Neptune and Triton. Science 246 (4936): 1459–1456.
  51. Template:Cite doi
  52. Stanley, Sabine (11 March 2004). Convective-region geometry as the cause of Uranus' and Neptune's unusual magnetic fields. Nature 428 (6979): 151–153.
  53. (1991) The magnetic field of Neptune. Journal of Geophysics Research 96: 19,023–42.
  54. 54.0 54.1 54.2 54.3 Ness, N. F. (1989). Magnetic Fields at Neptune. Science 246 (4936): 1473–1478.
  55. Russell, C. T. (1997). Neptune: Magnetic Field and Magnetosphere. University of California, Los Angeles. Retrieved 10 August 2006.
  56. Cruikshank, Dale P. (1996). Neptune and Triton. University of Arizona Press, 703–804. ISBN 978-0-8165-1525-7. 
  57. Blue, Jennifer (8 December 2004). Nomenclature Ring and Ring Gap Nomenclature. Gazetteer of Planetary. USGS. Retrieved 28 February 2008.
  58. (1982) Evidence for a Ring System of Neptune. Bulletin of the American Astronomical Society 14.
  59. Goldreich, P. (1986). Towards a theory for Neptune's arc rings. Astronomical Journal 92: 490–494.
  60. Nicholson, P. D. et al. (1990). Five Stellar Occultations by Neptune: Further Observations of Ring Arcs. Icarus 87 (1).
  61. Missions to Neptune. The Planetary Society (2007). Archived from the original on 2010-02-11. Retrieved 11 October 2007.
  62. Template:Cite news
  63. Cox, Arthur N. (2001). Allen's Astrophysical Quantities. Springer. ISBN 0-387-98746-0. 
  64. Munsell, Kirk (13 November 2007). Planets: Neptune: Rings. Solar System Exploration. NASA. Retrieved 29 February 2008.
  65. Salo, Heikki (1998). Neptune's Partial Rings: Action of Galatea on Self-Gravitating Arc Particles. Science 282 (5391): 1102–1104.
  66. Neptune's rings are fading away. New Scientist (26 March 2005). Retrieved 6 August 2007.
  67. 67.0 67.1 Lavoie, Sue (16 February 2000). PIA02245: Neptune's blue-green atmosphere. NASA JPL. Retrieved 28 February 2008.
  68. Lavoie, Sue (8 January 1998). PIA01142: Neptune Scooter. NASA. Retrieved 26 March 2006.
  69. (1989) Neptune's wind speeds obtained by tracking clouds in Voyager 2 images. Science 245 (4924): 1367–1369.
  70. 70.0 70.1 Burgess (1991):64–70.
  71. Orton, G. S., Encrenaz T., Leyrat C., Puetter, R. and Friedson, A. J. (2007). Evidence for methane escape and strong seasonal and dynamical perturbations of Neptune's atmospheric temperatures. Astronomy and Astrophysics 473: L5–L8.
  72. Template:Cite news
  73. 73.0 73.1 Template:Cite news
  74. Hammel, H. B. (1995). Hubble Space Telescope Imaging of Neptune's Cloud Structure in 1994. Science 268 (5218): 1740–1742.
  75. Lavoie, Sue (29 January 1996). PIA00064: Neptune's Dark Spot (D2) at High Resolution. NASA JPL. Retrieved 28 February 2008.
  76. S. G., Gibbard (2003). The altitude of Neptune cloud features from high-spatial-resolution near-infrared spectra. Icarus 166 (2): 359–374.
  77. Stratman, P. W. (2001). EPIC Simulations of Bright Companions to Neptune's Great Dark Spots. Icarus 151 (2): 275–285.
  78. (2000) The unusual dynamics of new dark spots on Neptune. Bulletin of the American Astronomical Society 32.
  79. Happy birthday Neptune. ESA/Hubble. Retrieved 13 July 2011.
  80. Williams, Sam (24 November 2004). Heat Sources Within the Giant Planets.
  81. Lindal, Gunnar F. (1992). The atmosphere of Neptune – an analysis of radio occultation data acquired with Voyager 2. Astronomical Journal 103: 967–982.
  82. Class 12 – Giant Planets – Heat and Formation. 3750 – Planets, Moons & Rings. Colorado University, Boulder (2004). Retrieved 13 March 2008.
  83. (1991) The albedo, effective temperature, and energy balance of Neptune, as determined from Voyager data. Journal of Geophysical Research Supplement 96: 18,921–18,930.
  84. Imke de Pater and Jack J. Lissauer (2001), Planetary Sciences, 1st edition, page 224.
  85. Jean Meeus, Astronomical Algorithms (Richmond, VA: Willmann-Bell, 1998) 273. Supplemented by further use of VSOP87. The last three aphelia were 30.33 AU, the next is 30.34 AU. The perihelia are even more stable at 29.81 AU
  86. Template:Cite news
  87. Neptune Completes First Orbit Since Discovery: 11th July 2011 (at 21:48 U.T.±15min) (1 July 2011). Retrieved 10 July 2011.
  88. 88.0 88.1 Munsell, K. (13 November 2007). Neptune: Facts & Figures. NASA. Retrieved 14 August 2007.
  89. Nancy Atkinson (26 August 2010). Clearing the Confusion on Neptune’s Orbit. Universe Today. Retrieved 2011-07-10. (Bill Folkner at JPL)
  90. 90.0 90.1 Anonymous (16 November 2007). Horizons Output for Neptune 2010–2011. Retrieved 25 February 2008.—Numbers generated using the Solar System Dynamics Group, Horizons On-Line Ephemeris System.
  91. Williams, David R. (6 January 2005). Planetary Fact Sheets. NASA. Retrieved 28 February 2008.
  92. Hubbard, W. B. (1991). Interior Structure of Neptune: Comparison with Uranus. Science 253 (5020): 648–651.
  93. Stern, S. Alan (1997). Collisional Erosion in the Primordial Edgeworth-Kuiper Belt and the Generation of the 30–50 AU Kuiper Gap. The Astrophysical Journal 490 (2): 879–882.
  94. Petit, Jean-Marc (1999). Large Scattered Planetesimals and the Excitation of the Small Body Belts. Icarus 141 (2).
  95. List Of Transneptunian Objects. Minor Planet Center. Retrieved 25 October 2010.
  96. Jewitt, David (2004). The Plutinos. UCLA. Retrieved 28 February 2008.
  97. Varadi, F. (1999). Periodic Orbits in the 3:2 Orbital Resonance and Their Stability. The Astronomical Journal 118 (5): 2526–2531.
  98. John Davies (2001). Beyond Pluto: Exploring the outer limits of the solar system. Cambridge University Press. ISBN 0-521-80019-6. 
  99. Chiang, E. I. (2003). Resonance Occupation in the Kuiper Belt: Case Examples of the 5 : 2 and Trojan Resonances. The Astronomical Journal 126: 430–443.
  100. Template:Wikilink (10 September 2010). Detection of a Trailing (L5) Neptune Trojan. Science 329 (5997).
  101. 101.0 101.1 de la Fuente Marcos & de la Fuente Marcos (2012). (309239) 2007 RW10: a large temporary quasi-satellite of Neptune. Astronomy and Astrophysics Letters 545: L9.
  102. Thommes, Edward W. (2001). The formation of Uranus and Neptune among Jupiter and Saturn. The Astronomical Journal 123 (5): 2862–2883.
  103. Hansen, Kathryn (7 June 2005). Orbital shuffle for early solar system. Geotimes. Retrieved 26 August 2007.
  104. Crida, A. (2009). Solar System formation. Reviews in Modern Astronomy 21.
  105. Desch, S. J. (2007). Mass Distribution and Planet Formation in the Solar Nebula. The Astrophysical Journal 671 (1): 878–893.
  106. Smith, R. (2009). Resolved debris disc emission around η Telescopii: a young solar system or ongoing planet formation?. Astronomy and Astrophysics 493 (1): 299–308.
  107. Hubble Space Telescope discovers fourteenth tiny moon orbiting Neptune | Space, Military and Medicine. (2013-07-16). Retrieved on 2013-07-28.
  108. Agnor, Craig B. (2006). Neptune's capture of its moon Triton in a binary–planet gravitational encounter. Nature 441 (7090): 192–194.
  109. (1989) Tidal evolution in the Neptune-Triton system. Astronomy and Astrophysics 219 (1–2): L23–L26.
  110. Template:Cite news
  111. Nelson, R. M.; Smythe, W. D.; Wallis, B. D.; Horn, L. J.; Lane, A. L.; Mayo, M. J. (1990). Temperature and Thermal Emissivity of the Surface of Neptune's Satellite Triton. Science 250 (4979): 429–431.
  112. Brown, Michael E.. The Dwarf Planets. California Institute of Technology, Department of Geological Sciences. Retrieved 9 February 2008.
  113. Template:Cite doi
  114. Template:Cite news
  115. 115.0 115.1 Espenak, Fred (20 July 2005). Twelve Year Planetary Ephemeris: 1995–2006. NASA. Retrieved 1 March 2008.
  116. See the respective articles for magnitude data.
  117. Moore (2000):207.
  118. In 1977, for example, even the rotation period of Neptune remained uncertain. Cruikshank, D. P. (1 March 1978). On the rotation period of Neptune. Astrophysical Journal, Part 2 – Letters to the Editor 220: L57–L59.
  119. Max, C. (1999). Adaptive Optics Imaging of Neptune and Titan with the W.M. Keck Telescope. Bulletin of the American Astronomical Society 31.
  120. (1999) High-Resolution Infrared Imaging of Neptune from the Keck Telescope. Icarus 156 (1): 1–15.
  121. Phillips, Cynthia (5 August 2003). Fascination with Distant Worlds. SETI Institute. Archived from the original on 3 November 2007. Retrieved 3 October 2007.
  122. 122.0 122.1 Burgess (1991):46–55.
  123. (2004) Outstanding Science in the Neptune System From an Aerocaptured Vision Mission. Bulletin of the American Astronomical Society 36.
  124. 124.0 124.1 124.2 Argo - A Voyage Through the Outer Solar System


Further readingEdit

External linksEdit

Template:Sister project links

Template:Neptune Template:Solar System Template:Atmospheres

Template:Featured articleTemplate:Link FA Template:Link FA

Ad blocker interference detected!

Wikia is a free-to-use site that makes money from advertising. We have a modified experience for viewers using ad blockers

Wikia is not accessible if you’ve made further modifications. Remove the custom ad blocker rule(s) and the page will load as expected.