Neptune

Neptune

The picture shows the Great Dark Spot and its companion bright smudge; on the west limb the fast moving bright feature called Scooter and the little dark spot are visible.
Discovery
Discovery date 23 September 1846[1]
Designations
Pronunciation /ˈnɛptuːn/
/ˈnɛptjuːn/[2]
Adjectives Neptunian
Orbital characteristics[3][lower-alpha 1]
Epoch J2000
Aphelion 30.33 AU
(4,540 Gm)
Perihelion 29.81 AU
(4,460 Gm)
30.110387 AU
(4,504.45 Gm)
Eccentricity 0.009456
164.8 yr
60,182 d
89,666 Neptunian solar days[4]
367.49 days[5]
5.43 km/s[5]
256.228°
Inclination 1.767975° to ecliptic
6.43° to Sun's equator
0.72° to invariable plane[6]
131.784°
276.336°
Known satellites 14
Physical characteristics
Mean radius
 24,622±19 km[7][lower-alpha 2]
Equatorial radius
 24,764±15 km[7][lower-alpha 2]
3.883 Earths
Polar radius
 24,341±30 km[7][lower-alpha 2]
3.829 Earths
Flattening 0.0171±0.0013
7.6183×109 km2[8][lower-alpha 2]
14.98 Earths
Volume 6.254×1013 km3[5][lower-alpha 2]
57.74 Earths
Mass 1.0243×1026 kg[5]
17.147 Earths
5.15×10−5 Suns
Mean density
 1.638 g/cm3[5][lower-alpha 3]
11.15 m/s2[5][lower-alpha 2]
1.14 g
0.23[9] (estimate)
23.5 km/s[5][lower-alpha 2]
0.6713 day[5]
16 h 6 min 36 s
Equatorial rotation velocity
 2.68 km/s
9,660 km/h
28.32° (to orbit)[5]
North pole right ascension
 19h 57m 20s[7]
299.3°
North pole declination
 42.950°[7]
Albedo

0.290 (bond)

0.41 (geom.)[5]
Surface temp. min mean max
1 bar level 72 K (−201 °C)[5]
0.1 bar (10 kPa) 55 K[5]
8.02 to 7.78[5][10]
2.2–2.4″[5][10]
Atmosphere[5]
19.7 ± 0.6 km
Composition by volume


Gases:
80 ± 3.2% hydrogen (H2)
19 ± 3.2% helium (He)
1.5 ± 0.5% methane (CH4)
~0.019% hydrogen deuteride (HD)
~0.00015% ethane (C2H6)
Ices:
ammonia (NH3)
water (H2O)
ammonium hydrosulfide (NH4SH)

methane ice (?) (CH4•5.75H2O)

    Neptune is the eighth and farthest known planet from the Sun in the Solar System. In the Solar System, it is the fourth-largest planet by diameter, the third-most-massive planet, and the densest giant planet. 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 and slightly larger than Neptune.[lower-alpha 4] Neptune orbits the Sun once every 164.8 years at an average distance of 30.1 astronomical units (4.50×109 km). It is named after the Roman god of the sea and has the astronomical symbol ♆, a stylised version of the god Neptune's trident.

    Neptune is not visible to the unaided eye and is the only planet in the Solar System 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 with a telescope on 23 September 1846[1] by Johann Galle within a degree of the position predicted by Urbain Le Verrier. Its largest moon, Triton, was discovered shortly thereafter, though none of the planet's remaining known 14 moons were located telescopically until the 20th century. The planet's distance from Earth gives it a very small apparent size, making it challenging to study with Earth-based telescopes. Neptune was visited by Voyager 2, when it flew by the planet on 25 August 1989.[11] The advent of the Hubble Space Telescope and large ground-based telescopes with adaptive optics has recently allowed for additional detailed observations from afar.

    Like Jupiter and Saturn, Neptune's atmosphere is composed primarily of hydrogen and helium, along with traces of hydrocarbons and possibly nitrogen, but it contains a higher proportion of "ices" such as water, ammonia, and methane. However, its interior, like that of Uranus, is primarily composed of ices and rock,[12] which is why Uranus and Neptune are normally considered "ice giants" to emphasise this distinction.[13] Traces of methane in the outermost regions in part account for the planet's blue appearance.[14]

    In contrast to the hazy, relatively featureless atmosphere of Uranus, Neptune's atmosphere has active and visible weather patterns. For example, at the time of the Voyager 2 flyby in 1989, the planet's southern hemisphere had 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 (580 m/s; 1,300 mph).[15] 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 (5,100 °C).[16][17] Neptune has a faint and fragmented ring system (labelled "arcs"), which was discovered in 1982, then later confirmed by Voyager 2.[18]

    History

    Discovery

    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;[19] hence, he is not credited with Neptune's discovery. At his first observation in December 1612, Neptune was almost 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.[20] 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.[21]

    In 1821, Alexis Bouvard published astronomical tables of the orbit of Neptune's neighbour Uranus.[22] Subsequent observations revealed substantial deviations from the tables, leading Bouvard to hypothesise that an unknown body was perturbing the orbit through gravitational interaction.[23] 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.[24][25]

    Urbain Le Verrier

    In 1845–46, Urbain Le Verrier, independently of Adams, developed his own calculations but aroused no 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.[23][26]

    Meanwhile, 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. On the evening of 23 September 1846, the day Galle received the letter, he discovered Neptune within 1° of where Le Verrier had predicted it to be, about 12° from Adams' prediction. Challis later realised that he had observed the planet twice, on 4 and 12 August, but did not recognise it as a planet because he lacked an up-to-date star map and was distracted by his concurrent work on comet observations.[23][27]

    In the wake of the discovery, there was much nationalistic rivalry between the French and the British over who 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.[28] 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."[29]

    Naming

    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.[30]

    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.[31] 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.[32] French almanacs quickly reintroduced the name Herschel for Uranus, after that planet's discoverer Sir William Herschel, and Leverrier for the new planet.[33]

    Struve came out in favour of the name Neptune on 29 December 1846, to the Saint Petersburg Academy of Sciences.[34] 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.[35]

    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. However, in Chinese, Japanese, and Korean, the planet's name was translated as "sea king star" (海王星), because Neptune was the god of the sea.[36] In Mongolian, Neptune is called Dalain Van (Далайн ван), reflecting its namesake god's role as the ruler of the sea. In modern Greek the planet is called Poseidon (Ποσειδώνας, Poseidonas), the Greek counterpart of Neptune.[37] In Hebrew, "Rahab" (רהב), from a Biblical sea monster mentioned in the Book of Psalms, was selected in a vote managed by the Academy of the Hebrew Language in 2009 as the official name for the planet, even though the existing Latin term "Neptun" (נפטון) is commonly used.[38][39] In Māori, the planet is called Tangaroa, named after the Māori god of the sea.[40] In Nahuatl, the planet is called Tlāloccītlalli, named after the rain god Tlāloc.[40] In Thai, Neptune is referred both by its Westernised name Dao Nepjun (ดาวเนปจูน), and is also named Dao Ketu (ดาวเกตุ, "Star of Ketu"), after the descending lunar node Ketu (केतु) who plays a role in Hindu astrology.

    Status

    From its discovery in 1846 until the subsequent discovery of Pluto in 1930, Neptune was the farthest known planet. When Pluto was discovered, it was considered a planet, and Neptune thus became the second-farthest known planet, except for a 20-year period between 1979 and 1999 when Pluto's elliptical orbit brought it closer than Neptune to the Sun.[41] The discovery of the Kuiper belt in 1992 led many astronomers to debate whether Pluto should be considered a planet or as part of the Kuiper belt.[42][43] 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 outermost known planet in the Solar System.[44]

    Physical characteristics

    A size comparison of Neptune and Earth

    Neptune's mass of 1.0243×1026 kg[5] is intermediate between Earth and the larger gas giants: it is 17 times that of Earth but just 1/19th that of Jupiter.[lower-alpha 5] Its gravity at 1 bar is 11.15 m/s2, 1.14 times the surface gravity of Earth,[45] and surpassed only by Jupiter.[46] Neptune's equatorial radius of 24,764 km[7] is nearly four times that of Earth. Neptune, like Uranus, is an ice giant, a subclass of giant planet, due to their smaller size and higher concentrations of volatiles relative to Jupiter and Saturn.[47] In the search for extrasolar planets, Neptune has been used as a metonym: discovered bodies of similar mass are often referred to as "Neptunes",[48] just as scientists refer to various extrasolar bodies as "Jupiters".

    Internal structure

    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.[16]

    The internal structure of Neptune:
    1. Upper atmosphere, top clouds
    2. Atmosphere consisting of hydrogen, helium and methane gas
    3. Mantle consisting of water, ammonia and methane ices
    4. Core consisting of rock (silicates and nickel–iron)

    The mantle is equivalent to 10 to 15 Earth masses and is rich in water, ammonia and methane.[1] As is customary in planetary science, this mixture is referred to as icy even though it is a hot, dense fluid. This fluid, which has a high electrical conductivity, is sometimes called a water–ammonia ocean.[49] The mantle may consist of a layer of ionic water in which 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.[50] At a depth of 7,000 km, the conditions may be such that methane decomposes into diamond crystals that rain downwards like hailstones.[51] Very-high-pressure experiments at the Lawrence Livermore National Laboratory suggest that the base of the mantle may be an ocean of liquid carbon with floating solid 'diamonds'.[52][53][54]

    The core of Neptune is likely composed of iron, nickel and silicates, with an interior model giving a mass about 1.2 times that of Earth.[55] 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.[16][17]

    Atmosphere

    Combined colour and near-infrared image of Neptune, showing bands of methane in its atmosphere, and four of its moons, Proteus, Larissa, Galatea, and Despina.

    At high altitudes, Neptune's atmosphere is 80% hydrogen and 19% helium.[16] A trace amount of methane is also present. Prominent absorption bands of methane exist 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,[56] 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.[14]

    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, lies at a pressure of 0.1 bars (10 kPa).[13] The stratosphere then gives way to the thermosphere at a pressure lower than 10−5 to 10−4 bars (1 to 10 Pa).[13] The thermosphere gradually transitions to the exosphere.

    Bands of high-altitude clouds cast shadows on Neptune's lower cloud deck

    Models suggest that Neptune's troposphere is banded by clouds of varying compositions depending on altitude. The upper-level clouds lie 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 thought 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.[57]

    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.[58] 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.[59]

    Neptune's spectra suggest that its lower stratosphere is hazy due to condensation of products of ultraviolet photolysis of methane, such as ethane and ethyne.[13][16] The stratosphere is also home to trace amounts of carbon monoxide and hydrogen cyanide.[13][60] The stratosphere of Neptune is warmer than that of Uranus due to the elevated concentration of hydrocarbons.[13]

    For reasons that remain obscure, the planet's thermosphere is at an anomalously high temperature of about 750 K.[61][62] 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.[57][60]

    Magnetosphere

    Neptune 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 13,500 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)[57] resulting in a dynamo action.[63]

    The dipole component of the magnetic field at the magnetic equator of Neptune is about 14 microteslas (0.14 G).[64] The dipole magnetic moment of Neptune is about 2.2 × 1017 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.[65][66]

    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.[65]

    Climate

    The Great Dark Spot (top), Scooter (middle white cloud),[67] and the Small Dark Spot (bottom), with contrast exaggerated.

    Neptune's weather is characterised by extremely dynamic storm systems, with winds reaching speeds of almost 600 m/s (2,200 km/h; 1,300 mph)—nearly reaching supersonic flow.[15] 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.[68] At the cloud tops, the prevailing winds range in speed from 400 m/s along the equator to 250 m/s at the poles.[57] Most of the winds on Neptune move in a direction opposite the planet's rotation.[69] The general pattern of winds showed prograde rotation at high latitudes vs. retrograde rotation at lower latitudes. The difference in flow direction is thought to be a "skin effect" and not due to any deeper atmospheric processes.[13] At 70° S latitude, a high-speed jet travels at a speed of 300 m/s.[13]

    Neptune differs from Uranus in its typical level of meteorological activity. Voyager 2 observed weather phenomena on Neptune during its 1989 flyby,[70] but no comparable phenomena on Uranus during its 1986 fly-by.

    The abundance of methane, ethane and acetylene 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.[13]

    In 2007, it was discovered that the upper troposphere of Neptune's south pole was about 10 K warmer than the rest of its atmosphere, which averages approximately 73 K (−200 °C). The temperature differential is enough to let methane, which elsewhere is frozen in the troposphere, escape into the stratosphere near the pole.[71] 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]

    Storms

    The Great Dark Spot, as imaged by Voyager 2

    In 1989, the Great Dark Spot, an anti-cyclonic storm system spanning 13,000 × 6,600 km,[70] 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 Neptune's northern hemisphere.[74]

    The Scooter is another storm, a white cloud group farther south than the Great Dark Spot. This nickname first arose during the months leading up to the Voyager 2 encounter in 1989, when they were observed moving at speeds faster than the Great Dark Spot (and images acquired later would subsequently reveal the presence of clouds moving even faster than those that had initially been detected by Voyager 2).[69] The Small Dark Spot is a southern cyclonic storm, the second-most-intense storm observed during the 1989 encounter. It was initially 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.[58] 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 heating

    Four images taken a few hours apart with the NASA/ESA Hubble Space Telescope's Wide Field Camera 3[79]

    Neptune's more varied weather when compared to Uranus is due in part to its higher internal heating. Although Neptune lies over 50% farther from the Sun than Uranus, and receives only 40% its amount of sunlight,[13] 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 rotation

    Neptune (red arc) completes one orbit around the Sun (centre) for every 164.79 orbits of Earth. The light blue object represents Uranus.

    The average distance between Neptune and the Sun is 4.50 billion km (about 30.1 astronomical units (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.[8][88][89]

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

    The axial tilt of Neptune is 28.32°,[90] which is similar to the tilts of Earth (23°) and Mars (25°). As a result, Neptune experiences similar seasonal changes to Earth. 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.[8] 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,[91] and it results in strong latitudinal wind shear.[58]

    Orbital resonances

    A diagram showing the major orbital resonances in the Kuiper belt caused by Neptune: the highlighted regions are the 2:3 resonance (plutinos), the nonresonant "classical belt" (cubewanos), and the 1:2 resonance (twotinos).

    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.[92] 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.[93]

    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,[94] 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.[95] Although Pluto crosses Neptune's orbit regularly, the 2:3 resonance ensures they can never collide.[96] The 3:4, 3:5, 4:7 and 2:5 resonances are less populated.[97]

    Neptune has a number of known trojan objects occupying both the Sun–Neptune L4 and L5 Lagrangian points—gravitationally stable regions leading and trailing Neptune in its orbit, respectively.[98] 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 object identified as associated with Neptune's trailing L5 Lagrangian point was 2008 LC18.[99] Neptune also has a temporary quasi-satellite, (309239) 2007 RW10.[100] 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.[100]

    Formation and migration

    A simulation showing the outer planets and Kuiper belt: a) before Jupiter and Saturn reached a 2:1 resonance; b) after inward scattering of Kuiper belt objects following the orbital shift of Neptune; c) after ejection of scattered Kuiper belt bodies by Jupiter

    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 formation. One is that the ice giants were not formed 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.[47]

    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.[101] 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.[102] The current most widely accepted[103][104][105] 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.

    Moons

    Natural-colour view of Neptune with Proteus (top), Larissa (lower right), and Despina (left), from the Hubble Space Telescope

    Neptune has 14 known moons.[5][106] Triton is the largest Neptunian moon, comprising more than 99.5% of the mass in orbit around Neptune,[lower-alpha 6] and it is the only one massive enough to be spheroidal. Triton was 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.[107] 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.[108] In 1989, Triton was the coldest object that had yet been measured in the Solar System,[109] with estimated temperatures of 38 K (−235 °C).[110]

    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 7]

    Neptune's moon Proteus

    From July to September 1989, Voyager 2 discovered six moons of Neptune.[111] 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, Larissa 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.[35]

    Planetary rings

    Neptune's rings

    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.[115] 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.[116]

    The first of these planetary rings was detected in 1968 by a team led by Edward Guinan.[18][117] In the early 1980s, analysis of this data along with newer observations led to the hypothesis that this ring might be incomplete.[118] 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.[119] Images from Voyager 2 in 1989 settled the issue by showing several faint rings.

    The outermost ring, Adams, contains five prominent arcs now named Courage, Liberté, Egalité 1, Egalité 2 and Fraternité (Courage, Liberty, Equality and Fraternity).[120] 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 estimate that the arcs are corralled into their current form by the gravitational effects of Galatea, a moon just inward from the ring.[121][122]

    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.[123]

    Observation

    With an apparent magnitude between +7.7 and +8.0, Neptune is never visible to the naked eye[5][10] and 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.[124] A telescope or strong binoculars will resolve Neptune as a small blue disk, similar in appearance to Uranus.[125]

    Because of the distance of Neptune from Earth, its angular diameter only ranges from 2.2 to 2.4 arcseconds,[5][10] the smallest of the Solar System planets. Its small apparent size makes it challenging to study it visually. Most telescopic data was fairly limited until the advent of the Hubble Space Telescope and large ground-based telescopes with adaptive optics (AO).[126][127][128] The first scientifically useful observation of Neptune from ground-based telescopes using adaptive optics, was commenced in 1997 from Hawaii.[129] Neptune is currently entering its spring and summer season and has been shown to be heating up, with increased atmospheric activity and brightness as a consequence. Combined with technological advancements, ground-based telescopes with adaptive optics are recording increasingly more detailed images of it. Both Hubble and the adaptive-optics telescopes on Earth have made many new discoveries within the Solar System since the mid-1990s, with a large increase in the number of known satellites and moons around the outer planet, among others. In 2004 and 2005, five new small satellites of Neptune with diameters between 38 and 61 kilometres were discovered.[130]

    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.[89]

    Observation of Neptune in the radio-frequency band shows that it is a source of both continuous emission and irregular bursts. Both sources are thought to originate from its rotating magnetic field.[57] 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.[131]

    Exploration

    A Voyager 2 mosaic of Triton

    Voyager 2 is the only spacecraft that has visited Neptune. The spacecraft's closest approach to the planet 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.[132]

    During the encounter, signals from the spacecraft required 246 minutes to reach Earth. Hence, for the most part, Voyager 2's mission relied on preloaded commands for the Neptune encounter. The spacecraft performed a near-encounter with the moon Nereid before it came within 4,400 km of Neptune's atmosphere on 25 August, then passed close to the planet's largest moon Triton later the same day.[133]

    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. Neptune's rotation period was determined using measurements of radio emissions and 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.[111][133]

    The flyby also provided the first accurate measurement of Neptune's mass which was found to be 0.5 percent less than previously calculated. The new figure disproved the hypothesis that an undiscovered Planet X acted upon the orbits of Neptune and Uranus.[134][135]

    After the Voyager 2 flyby mission, the next step in scientific exploration of the Neptunian system, is considered to be a Flagship orbital mission.[136] Such a hypothetical mission is envisioned to be possible in the late 2020s or early 2030s.[136] However, there have been a couple of discussions to launch Neptune missions sooner. In 2003, there was a proposal in NASA's "Vision Missions Studies" for a "Neptune Orbiter with Probes" mission that does Cassini-level science.[137] Another, more recent proposal was for Argo, a flyby spacecraft to be launched in 2019, that would visit Jupiter, Saturn, Neptune, and a Kuiper belt object. The focus would be on Neptune and its largest moon Triton to be investigated around 2029.[138] The proposed New Horizons 2 mission (which was later scrapped) might also have done a close flyby of the Neptunian system.

    See also

    Notes

    1. ↑ 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.
    2. 1 2 3 4 5 6 7 Refers to the level of 1 bar (100 kPa) atmospheric pressure
    3. ↑ Based on the volume within the level of 1 bar atmospheric pressure
    4. ↑ Neptune is denser and physically smaller than Uranus because Neptune's greater mass gravitationally compresses the atmosphere more.
    5. ↑ The mass of Earth is 5.9736×1024 kg, giving a mass ratio
      The mass of Uranus is 8.6810×1025 kg, giving a mass ratio
      The mass of Jupiter is 1.8986×1027 kg, giving a mass ratio
      Mass values from Williams, David R. (29 November 2007). "Planetary Fact Sheet – Metric". NASA. Retrieved 13 March 2008.
    6. ↑ 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.
    7. ↑

    References

    1. 1 2 3 Hamilton, Calvin J. (4 August 2001). "Neptune". Views of the Solar System. 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. ↑ Yeomans, Donald K. "HORIZONS Web-Interface for Neptune Barycenter (Major Body=8)". JPL Horizons On-Line Ephemeris System. 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)".)
    4. ↑ Seligman, Courtney. "Rotation Period and Day Length". Retrieved 13 August 2009.
    5. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 Williams, David R. (1 September 2004). "Neptune Fact Sheet". NASA. Retrieved 14 August 2007.
    6. ↑ "The MeanPlane (Invariable plane) of the Solar System passing through the barycenter". 3 April 2009. Archived from the original on 14 May 2009. Retrieved 10 April 2009. (produced with Solex 10 Archived 29 April 2009 at WebCite written by Aldo Vitagliano; see also Invariable plane)
    7. 1 2 3 4 5 6 Seidelmann, P. Kenneth; Archinal, Brent A.; A'Hearn, Michael F.; et al. (2007). "Report of the IAU/IAG Working Group on cartographic coordinates and rotational elements: 2006". Celestial Mechanics and Dynamical Astronomy. 98 (3): 155–180. Bibcode:2007CeMDA..98..155S. doi:10.1007/s10569-007-9072-y.
    8. 1 2 3 Munsell, K.; Smith, H.; Harvey, S. (13 November 2007). "Neptune: Facts & Figures". NASA. Retrieved 14 August 2007.
    9. ↑ de Pater, Imke; Lissauer, Jack J. (2015). Planetary Sciences (2nd updated ed.). New York: Cambridge University Press. p. 250. ISBN 978-0521853712.
    10. 1 2 3 4 Espenak, Fred (20 July 2005). "Twelve Year Planetary Ephemeris: 1995–2006". NASA. Retrieved 1 March 2008.
    11. ↑ Chang, Kenneth (18 October 2014). "Dark Spots in Our Knowledge of Neptune". New York Times. Retrieved 21 October 2014.
    12. ↑ Podolak, M.; Weizman, A.; Marley, M. (December 1995). "Comparative models of Uranus and Neptune". Planetary and Space Science. 43 (12): 1517–1522. Bibcode:1995P&SS...43.1517P. doi:10.1016/0032-0633(95)00061-5.
    13. 1 2 3 4 5 6 7 8 9 10 Lunine, Jonathan I. (September 1993). "The Atmospheres of Uranus and Neptune". Annual Review of Astronomy and Astrophysics. 31: 217–263. Bibcode:1993ARA&A..31..217L. doi:10.1146/annurev.aa.31.090193.001245.
    14. 1 2 Munsell, Kirk; Smith, Harman; Harvey, Samantha (13 November 2007). "Neptune overview". Solar System Exploration. NASA. Archived from the original on 3 March 2008. Retrieved 20 February 2008.
    15. 1 2 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. PMID 17847386. doi:10.1126/science.251.4996.929.
    16. 1 2 3 4 5 Hubbard, W. B. (1997). "Neptune's Deep Chemistry". Science. 275 (5304): 1279–1280. PMID 9064785. doi:10.1126/science.275.5304.1279.
    17. 1 2 Nettelmann, N.; French, M.; Holst, B.; Redmer, R. "Interior Models of Jupiter, Saturn and Neptune" (PDF). University of Rostock. Archived from the original (PDF) on 18 July 2011. Retrieved 25 February 2008.
    18. 1 2 Wilford, John N. (10 June 1982). "Data Shows 2 Rings Circling Neptune". The New York Times. Retrieved 29 February 2008.
    19. ↑ Hirschfeld, Alan (2001). Parallax: The Race to Measure the Cosmos. New York, New York: Henry Holt. ISBN 978-0-8050-7133-7.
    20. ↑ Littmann, Mark; Standish, E. M. (2004). Planets Beyond: Discovering the Outer Solar System. Courier Dover Publications. ISBN 978-0-486-43602-9.
    21. ↑ Britt, Robert Roy (2009). "Galileo discovered Neptune, new theory claims". MSNBC News. Retrieved 10 July 2009.
    22. ↑ Bouvard, A. (1821). Tables astronomiques publiées par le Bureau des Longitudes de France. Paris: Bachelier.
    23. 1 2 3 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. Bibcode:1846MNRAS...7..121A. doi:10.1002/asna.18470251002.
    24. ↑ O'Connor, John J.; Robertson, Edmund F. (2006). "John Couch Adams' account of the discovery of Neptune". University of St Andrews. Retrieved 18 February 2008.
    25. ↑ 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: 149–152. Bibcode:1846MNRAS...7..149A. doi:10.1093/mnras/7.9.149.
    26. ↑ 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. Bibcode:1846MNRAS...7..145C. doi:10.1093/mnras/7.9.145.
    27. ↑ 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: 153. Bibcode:1846MNRAS...7..153G. doi:10.1093/mnras/7.9.153.
    28. ↑ 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.
    29. ↑ William Sheehan; Nicholas Kollerstrom; Craig B. Waff (December 2004). "The Case of the Pilfered Planet – Did the British steal Neptune?". Scientific American. Retrieved 20 January 2011.
    30. ↑ Moore (2000):206
    31. ↑ Littmann, Mark (2004). Planets Beyond, Exploring the Outer Solar System. Courier Dover Publications. p. 50. ISBN 978-0-486-43602-9.
    32. ↑ Baum, Richard; Sheehan, William (2003). In Search of Planet Vulcan: The Ghost in Newton's Clockwork Universe. Basic Books. pp. 109–110. ISBN 978-0-7382-0889-3.
    33. ↑ Gingerich, Owen (1958). "The Naming of Uranus and Neptune". Astronomical Society of the Pacific Leaflets. 8: 9–15. Bibcode:1958ASPL....8....9G.
    34. ↑ Hind, J. R. (1847). "Second report of proceedings in the Cambridge Observatory relating to the new Planet (Neptune)". Astronomische Nachrichten. 25 (21): 309–314. Bibcode:1847AN.....25..309.. doi:10.1002/asna.18470252102.
    35. 1 2 Blue, Jennifer (17 December 2008). "Planet and Satellite Names and Discoverers". USGS. Retrieved 18 February 2008.
    36. ↑ "Planetary linguistics". nineplanets.org. Retrieved 8 April 2010.
    37. ↑ "Greek Names of the Planets". Retrieved 14 July 2012. Neptune or Poseidon as is its Greek name, was the God of the Seas. It is the eight planet from the sun... See also the Greek article about the planet.
    38. ↑ "Uranus and Neptune get Hebrew names at last", Haaretz.com
    39. ↑ "Hebrew names to Uranus and Neptune" Hayadan.org.il (Hebrew)
    40. 1 2 "Appendix 5: Planetary Linguistics", Nineplanets.org
    41. ↑ Long, Tony (21 January 2008). "Jan. 21, 1979: Neptune Moves Outside Pluto's Wacky Orbit". Wired. Retrieved 13 March 2008.
    42. ↑ Weissman, Paul R. (1995). "The Kuiper Belt". Annual Review of Astronomy and Astrophysics. 33: 327–357. Bibcode:1995ARA&A..33..327W. doi:10.1146/annurev.aa.33.090195.001551.
    43. ↑ "The Status of Pluto:A clarification". International Astronomical Union, Press release. 1999. Archived from the original on 15 June 2006. Retrieved 25 May 2006.
    44. ↑ "IAU 2006 General Assembly: Resolutions 5 and 6" (PDF). IAU. 24 August 2006.
    45. ↑ "Neptune Fact Sheet". NASA.
    46. ↑ Unsöld, Albrecht; Baschek, Bodo (2001). The New Cosmos: An Introduction to Astronomy and Astrophysics (5th ed.). Springer. p. 47. ISBN 978-3-540-67877-9. See Table 3.1.
    47. 1 2 Boss, Alan P. (2002). "Formation of gas and ice giant planets". Earth and Planetary Science Letters. 202 (3–4): 513–523. Bibcode:2002E&PSL.202..513B. doi:10.1016/S0012-821X(02)00808-7.
    48. ↑ Lovis, C.; Mayor, M.; Alibert Y.; Benz W. (18 May 2006). "Trio of Neptunes and their Belt". ESO. Retrieved 25 February 2008.
    49. ↑ Atreya, S.; Egeler, P.; Baines, K. (2006). "Water-ammonia ionic ocean on Uranus and Neptune?" (PDF). Geophysical Research Abstracts. 8: 05179.
    50. ↑ Weird water lurking inside giant planets, New Scientist,1 September 2010, Magazine issue 2776.
    51. ↑ Kerr, Richard A. (1999). "Neptune May Crush Methane Into Diamonds". Science. 286 (5437): 25a–25. PMID 10532884. doi:10.1126/science.286.5437.25a.
    52. ↑ Baldwin, Emily (21 January 2010). "Oceans of diamond possible on Uranus and Neptune". astronomynow.com. Archived from the original on 3 December 2013. Retrieved 6 February 2014.
    53. ↑ Bradley, D. K.; Eggert, J. H.; Hicks, D. G.; Celliers, P. M. (30 July 2004). "Shock Compressing Diamond to a Conducting Fluid" (PDF). Physical Review Letters. 93. doi:10.1103/physrevlett.93.195506. Retrieved 16 March 2016.
    54. ↑ Eggert, J. H.; Hicks, D. G.; Celliers, P. M.; Bradley, D. K.; et al. (8 November 2009). "Melting temperature of diamond at ultrahigh pressure". Nature Physics. 6 (40): 40–43. doi:10.1038/nphys1438. Retrieved 16 March 2016.
    55. ↑ Podolak, M.; Weizman, A.; Marley, M. (1995). "Comparative models of Uranus and Neptune". Planetary and Space Science. 43 (12): 1517–1522. Bibcode:1995P&SS...43.1517P. doi:10.1016/0032-0633(95)00061-5.
    56. ↑ Crisp, D.; Hammel, H. B. (14 June 1995). "Hubble Space Telescope Observations of Neptune". Hubble News Center. Retrieved 22 April 2007.
    57. 1 2 3 4 5 Elkins-Tanton, Linda T. (2006). Uranus, Neptune, Pluto, and the Outer Solar System. New York: Chelsea House. pp. 79–83. ISBN 978-0-8160-5197-7.
    58. 1 2 3 Max, C. E.; Macintosh, B. A.; Gibbard, S. G.; Gavel, D. T.; et al. (2003). "Cloud Structures on Neptune Observed with Keck Telescope Adaptive Optics". The Astronomical Journal. 125 (1): 364–375. Bibcode:2003AJ....125..364M. doi:10.1086/344943.
    59. ↑ Frances, Peter (2008). DK Universe. DK Publishing. pp. 196–201. ISBN 978-0-7566-3670-8.
    60. 1 2 Encrenaz, Thérèse (February 2003). "ISO observations of the giant planets and Titan: what have we learnt?". Planetary and Space Science. 51 (2): 89–103. Bibcode:2003P&SS...51...89E. doi:10.1016/S0032-0633(02)00145-9.
    61. ↑ Broadfoot, A.L.; Atreya, S.K.; Bertaux, J.L.; et al. (1999). "Ultraviolet Spectrometer Observations of Neptune and Triton" (PDF). Science. 246 (4936): 1459–66. Bibcode:1989Sci...246.1459B. PMID 17756000. doi:10.1126/science.246.4936.1459.
    62. ↑ Herbert, Floyd; Sandel, Bill R. (August–September 1999). "Ultraviolet observations of Uranus and Neptune". Planetary and Space Science. 47 (8–9): 1,119–1,139. Bibcode:1999P&SS...47.1119H. doi:10.1016/S0032-0633(98)00142-1.
    63. ↑ Stanley, Sabine; Bloxham, Jeremy (11 March 2004). "Convective-region geometry as the cause of Uranus' and Neptune's unusual magnetic fields". Nature. 428 (6979): 151–153. Bibcode:2004Natur.428..151S. PMID 15014493. doi:10.1038/nature02376.
    64. ↑ Connerney, J. E. P.; Acuña, Mario H.; Ness, Norman F. (1991). "The magnetic field of Neptune". Journal of Geophysical Research. 96: 19,023–42. Bibcode:1991JGR....9619023C. doi:10.1029/91JA01165.
    65. 1 2 Ness, N. F.; Acuña, M. H.; Burlaga, L. F.; Connerney, J. E. P.; Lepping, R. P.; Neubauer, F. M. (1989). "Magnetic Fields at Neptune". Science. 246 (4936): 1473–1478. Bibcode:1989Sci...246.1473N. PMID 17756002. doi:10.1126/science.246.4936.1473.
    66. ↑ Russell, C. T.; Luhmann, J. G. (1997). "Neptune: Magnetic Field and Magnetosphere". University of California, Los Angeles. Retrieved 10 August 2006.
    67. ↑ Lavoie, Sue (8 January 1998). "PIA01142: Neptune Scooter". NASA. Retrieved 26 March 2006.
    68. ↑ Hammel, H. B.; Beebe, R. F.; De Jong, E. M.; Hansen, C. J.; et al. (1989). "Neptune's wind speeds obtained by tracking clouds in Voyager 2 images". Science. 245 (4924): 1367–1369. Bibcode:1989Sci...245.1367H. PMID 17798743. doi:10.1126/science.245.4924.1367.
    69. 1 2 Burgess (1991):64–70.
    70. 1 2 Lavoie, Sue (16 February 2000). "PIA02245: Neptune's blue-green atmosphere". NASA JPL. Retrieved 28 February 2008.
    71. ↑ Orton, G. S.; Encrenaz T.; Leyrat C.; Puetter, R.; et al. (2007). "Evidence for methane escape and strong seasonal and dynamical perturbations of Neptune's atmospheric temperatures". Astronomy and Astrophysics. 473: L5–L8. Bibcode:2007A&A...473L...5O. doi:10.1051/0004-6361:20078277.
    72. ↑ Orton, Glenn; Encrenaz, Thérèse (18 September 2007). "A Warm South Pole? Yes, On Neptune!". ESO. Retrieved 20 September 2007.
    73. 1 2 Villard, Ray; Devitt, Terry (15 May 2003). "Brighter Neptune Suggests A Planetary Change Of Seasons". Hubble News Center. Retrieved 26 February 2008.
    74. ↑ Hammel, H. B.; Lockwood, G. W.; Mills, J. R.; Barnet, C. D. (1995). "Hubble Space Telescope Imaging of Neptune's Cloud Structure in 1994". Science. 268 (5218): 1740–1742. Bibcode:1995Sci...268.1740H. PMID 17834994. doi:10.1126/science.268.5218.1740.
    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; de Pater, I.; Roe, H. G.; Martin, S.; et al. (2003). "The altitude of Neptune cloud features from high-spatial-resolution near-infrared spectra" (PDF). Icarus. 166 (2): 359–374. Bibcode:2003Icar..166..359G. doi:10.1016/j.icarus.2003.07.006. Retrieved 26 February 2008.
    77. ↑ Stratman, P. W.; Showman, A. P.; Dowling, T. E.; Sromovsky, L. A. (2001). "EPIC Simulations of Bright Companions to Neptune's Great Dark Spots" (PDF). Icarus. 151 (2): 275–285. Bibcode:1998Icar..132..239L. doi:10.1006/icar.1998.5918. Retrieved 26 February 2008.
    78. ↑ Sromovsky, L. A.; Fry, P. M.; Dowling, T. E.; Baines, K. H. (2000). "The unusual dynamics of new dark spots on Neptune". Bulletin of the American Astronomical Society. 32: 1005. Bibcode:2000DPS....32.0903S.
    79. ↑ "Happy birthday Neptune". ESA/Hubble. Retrieved 13 July 2011.
    80. ↑ Williams, Sam (24 November 2004). "Heat Sources Within the Giant Planets" (DOC). UC Berkeley. Retrieved 20 February 2008.
    81. ↑ Lindal, Gunnar F. (1992). "The atmosphere of Neptune – an analysis of radio occultation data acquired with Voyager 2". Astronomical Journal. 103: 967–982. Bibcode:1992AJ....103..967L. doi:10.1086/116119.
    82. ↑ "Class 12 – Giant Planets – Heat and Formation". 3750 – Planets, Moons & Rings. Colorado University, Boulder. 2004. Retrieved 13 March 2008.
    83. ↑ Pearl, J. C.; Conrath, B. J. (1991). "The albedo, effective temperature, and energy balance of Neptune, as determined from Voyager data". Journal of Geophysical Research: Space Physics. 96: 18,921–18,930. Bibcode:1991JGR....9618921P. doi:10.1029/91ja01087.
    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. ↑ McKie, Robin (9 July 2011). "Neptune's first orbit: a turning point in astronomy". The Guardian.
    87. ↑ "Neptune Completes First Orbit Since Discovery: 11th July 2011 (at 21:48 U.T.±15min)". 1 July 2011. Retrieved 10 July 2011.
    88. ↑ Nancy Atkinson (26 August 2010). "Clearing the Confusion on Neptune’s Orbit". Universe Today. Retrieved 10 July 2011. (Bill Folkner at JPL)
    89. 1 2 Anonymous (16 November 2007). "Horizons Output for Neptune 2010–2011". Archived from the original on 2 May 2013. Retrieved 25 February 2008.—Numbers generated using the Solar System Dynamics Group, Horizons On-Line Ephemeris System.
    90. ↑ Williams, David R. (6 January 2005). "Planetary Fact Sheets". NASA. Retrieved 28 February 2008.
    91. ↑ Hubbard, W. B.; Nellis, W. J.; Mitchell, A. C.; Holmes, N. C.; et al. (1991). "Interior Structure of Neptune: Comparison with Uranus". Science. 253 (5020): 648–651. Bibcode:1991Sci...253..648H. PMID 17772369. doi:10.1126/science.253.5020.648.
    92. ↑ Stern, S. Alan; Colwell, Joshua E. (1997). "Collisional Erosion in the Primordial Edgeworth-Kuiper Belt and the Generation of the 30–50 AU Kuiper Gap". The Astrophysical Journal. Geophysical, Astrophysical, and Planetary Sciences, Space Science Department, Southwest Research Institute. 490 (2): 879–882. Bibcode:1997ApJ...490..879S. doi:10.1086/304912.
    93. ↑ Petit, Jean-Marc; Morbidelli, Alessandro; Valsecchi, Giovanni B. (1999). "Large Scattered Planetesimals and the Excitation of the Small Body Belts" (PDF). Icarus. 141 (2): 367–387. Bibcode:1999Icar..141..367P. doi:10.1006/icar.1999.6166. Retrieved 23 June 2007.
    94. ↑ "List Of Transneptunian Objects". Minor Planet Center. Retrieved 25 October 2010.
    95. ↑ Jewitt, David (2004). "The Plutinos". UCLA. Retrieved 28 February 2008.
    96. ↑ Varadi, F. (1999). "Periodic Orbits in the 3:2 Orbital Resonance and Their Stability". The Astronomical Journal. 118 (5): 2526–2531. Bibcode:1999AJ....118.2526V. doi:10.1086/301088.
    97. ↑ John Davies (2001). Beyond Pluto: Exploring the outer limits of the solar system. Cambridge University Press. p. 104. ISBN 0-521-80019-6.
    98. ↑ Chiang, E. I.; Jordan, A. B.; Millis, R. L.; M. W. Buie; et al. (2003). "Resonance Occupation in the Kuiper Belt: Case Examples of the 5 : 2 and Trojan Resonances". The Astronomical Journal. 126: 430–443. Bibcode:2003AJ....126..430C. arXiv:astro-ph/0301458 Freely accessible. doi:10.1086/375207.
    99. ↑ Sheppard, Scott S.; Trujillo, Chadwick A. (10 September 2010). "Detection of a Trailing (L5) Neptune Trojan". Science. 329 (5997): 1304. Bibcode:2010Sci...329.1304S. PMID 20705814. doi:10.1126/science.1189666.
    100. 1 2 De La Fuente Marcos, C. & De La Fuente Marcos, R. (2012). "(309239) 2007 RW10: a large temporary quasi-satellite of Neptune". Astronomy and Astrophysics Letters. 545: L9. Bibcode:2012A&A...545L...9D. arXiv:1209.1577 Freely accessible. doi:10.1051/0004-6361/201219931.
    101. ↑ Thommes, Edward W.; Duncan, Martin J.; Levison, Harold F. (2001). "The formation of Uranus and Neptune among Jupiter and Saturn". The Astronomical Journal. 123 (5): 2862–2883. Bibcode:2002AJ....123.2862T. arXiv:astro-ph/0111290 Freely accessible. doi:10.1086/339975.
    102. ↑ Hansen, Kathryn (7 June 2005). "Orbital shuffle for early solar system". Geotimes. Retrieved 26 August 2007.
    103. ↑ Crida, A. (2009). "Solar System formation". Reviews in Modern Astronomy. 21: 3008. Bibcode:2009RvMA...21..215C. arXiv:0903.3008 Freely accessible. doi:10.1002/9783527629190.ch12.
    104. ↑ Desch, S. J. (2007). "Mass Distribution and Planet Formation in the Solar Nebula". The Astrophysical Journal. 671 (1): 878–893. Bibcode:2007ApJ...671..878D. doi:10.1086/522825.
    105. ↑ Smith, R.; L. J. Churcher; M. C. Wyatt; M. M. Moerchen; et al. (2009). "Resolved debris disc emission around η Telescopii: a young solar system or ongoing planet formation?". Astronomy and Astrophysics. 493 (1): 299–308. Bibcode:2009A&A...493..299S. arXiv:0810.5087 Freely accessible. doi:10.1051/0004-6361:200810706.
    106. ↑ Hubble Space Telescope discovers fourteenth tiny moon orbiting Neptune | Space, Military and Medicine. News.com.au (16 July 2013). Retrieved on 28 July 2013.
    107. ↑ Agnor, Craig B.; Hamilton, Douglas P. (2006). "Neptune's capture of its moon Triton in a binary–planet gravitational encounter". Nature. Nature Publishing Group. 441 (7090): 192–194. Bibcode:2006Natur.441..192A. PMID 16688170. doi:10.1038/nature04792.
    108. ↑ Chyba, Christopher F.; Jankowski, D. G.; Nicholson, P. D. (1989). "Tidal evolution in the Neptune-Triton system". Astronomy and Astrophysics. EDP Sciences. 219 (1–2): L23–L26. Bibcode:1989A&A...219L..23C.
    109. ↑ Wilford, John N. (29 August 1989). "Triton May Be Coldest Spot in Solar System". The New York Times. Retrieved 29 February 2008.
    110. ↑ Nelson, R. M.; Smythe, W. D.; Wallis, B. D.; Horn, L. J.; et al. (1990). "Temperature and Thermal Emissivity of the Surface of Neptune's Satellite Triton". Science. 250 (4979): 429–431. Bibcode:1990Sci...250..429N. PMID 17793020. doi:10.1126/science.250.4979.429.
    111. 1 2 Stone, E. C.; Miner, E. D. (1989). "The Voyager 2 Encounter with the Neptunian System". Science. 246 (4936): 1417–1421. Bibcode:1989Sci...246.1417S. PMID 17755996. doi:10.1126/science.246.4936.1417.
    112. ↑ Brown, Michael E. "The Dwarf Planets". California Institute of Technology, Department of Geological Sciences. Retrieved 9 February 2008.
    113. ↑ Holman, M. J.; Kavelaars, J. J.; Grav, T.; et al. (2004). "Discovery of five irregular moons of Neptune" (PDF). Nature. 430 (7002): 865–867. Bibcode:2004Natur.430..865H. PMID 15318214. doi:10.1038/nature02832. Retrieved 24 October 2011.
    114. ↑ "Five new moons for planet Neptune". BBC News. 18 August 2004. Retrieved 6 August 2007.
    115. ↑ Cruikshank, Dale P. (1996). Neptune and Triton. University of Arizona Press. pp. 703–804. ISBN 978-0-8165-1525-7.
    116. ↑ Blue, Jennifer (8 December 2004). "Nomenclature Ring and Ring Gap Nomenclature". Gazetteer of Planetary. USGS. Retrieved 28 February 2008.
    117. ↑ Guinan, E. F.; Harris, C. C.; Maloney, F. P. (1982). "Evidence for a Ring System of Neptune". Bulletin of the American Astronomical Society. 14: 658. Bibcode:1982BAAS...14..658G.
    118. ↑ Goldreich, P.; Tremaine, S.; Borderies, N. E. F. (1986). "Towards a theory for Neptune's arc rings". Astronomical Journal. 92: 490–494. Bibcode:1986AJ.....92..490G. doi:10.1086/114178.
    119. ↑ Nicholson, P. D.; et al. (1990). "Five Stellar Occultations by Neptune: Further Observations of Ring Arcs". Icarus. 87 (1): 1–39. Bibcode:1990Icar...87....1N. doi:10.1016/0019-1035(90)90020-A.
    120. ↑ Cox, Arthur N. (2001). Allen's Astrophysical Quantities. Springer. ISBN 0-387-98746-0.
    121. ↑ Munsell, Kirk; Smith, Harman; Harvey, Samantha (13 November 2007). "Planets: Neptune: Rings". Solar System Exploration. NASA. Retrieved 29 February 2008.
    122. ↑ Salo, Heikki; Hänninen, Jyrki (1998). "Neptune's Partial Rings: Action of Galatea on Self-Gravitating Arc Particles". Science. 282 (5391): 1102–1104. Bibcode:1998Sci...282.1102S. PMID 9804544. doi:10.1126/science.282.5391.1102.
    123. ↑ "Neptune's rings are fading away". New Scientist. 26 March 2005. Retrieved 6 August 2007.
    124. ↑ See the respective articles for magnitude data.
    125. ↑ Moore (2000):207.
    126. ↑ 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 Letters. University of Chicago Press. 220: L57–L59. Bibcode:1978ApJ...220L..57C. doi:10.1086/182636.
    127. ↑ Max, C.; MacIntosh, B.; Gibbard, S.; Roe, H.; et al. (1999). "Adaptive Optics Imaging of Neptune and Titan with the W.M. Keck Telescope". Bulletin of the American Astronomical Society. 31: 1512. Bibcode:1999BAAS...31.1512M.
    128. ↑ Nemiroff, R.; Bonnell, J., eds. (18 February 2000). "Neptune through Adaptive Optics". Astronomy Picture of the Day. NASA.
    129. ↑ First Ground-Based Adaptive Optics Observations of Neptune and Proteus Planetary & Space Science Vol. 45, No. 8, pp. 1031-1036, 1997
    130. ↑ Uranus and Neptune Reports on Astronomy 2003-2005, p. 147 f.
    131. ↑ Gibbard, S. G.; Roe, H.; de Pater, I.; Macintosh, B.; et al. (1999). "High-Resolution Infrared Imaging of Neptune from the Keck Telescope". Icarus. 156 (1): 1–15. Bibcode:2002Icar..156....1G. doi:10.1006/icar.2001.6766.
    132. ↑ Phillips, Cynthia (5 August 2003). "Fascination with Distant Worlds". SETI Institute. Archived from the original on 3 November 2007. Retrieved 3 October 2007.
    133. 1 2 Burgess (1991):46–55.
    134. ↑ Tom Standage (2000). The Neptune File: A Story of Astronomical Rivalry and the Pioneers of Planet Hunting. New York: Walker. p. 188. ISBN 978-0-8027-1363-6.
    135. ↑ Chris Gebhardt; Jeff Goldader (20 August 2011). "Thirty-four years after launch, Voyager 2 continues to explore". NASASpaceflight.
    136. 1 2 Clark, Stephen (25 August 2015). "Uranus, Neptune in NASA’s sights for new robotic mission". Spaceflight Now. Retrieved 7 September 2015.
    137. ↑ Spilker, T. R.; Ingersoll, A. P. (2004). "Outstanding Science in the Neptune System From an Aerocaptured Vision Mission". Bulletin of the American Astronomical Society. 36: 1094. Bibcode:2004DPS....36.1412S.
    138. ↑ Candice Hansen; et al. "Argo - A Voyage Through the Outer Solar System" (PDF). SpacePolicyOnline.com. Space and Technology Policy Group, LLC. Retrieved 5 August 2015.

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