Triton (moon)

Not to be confused with Titan (moon).
Triton

Discovery
Discovered by William Lassell
Discovery date October 10, 1846
Designations
Pronunciation /ˈtraɪtən/
Neptune I
Adjectives Tritonian
Orbital characteristics
354759 km
Eccentricity 0.000016[1]
−5.876854 d
(retrograde)[1][2]
4.39 km/s[lower-alpha 1]
Inclination 129.812° (to the ecliptic)
156.885° (to Neptune's equator)[3][4]
129.608° (to Neptune's orbit)
Satellite of Neptune
Physical characteristics
Mean radius
 1353.4±0.9 km[5] (0.2122 Earths)
23018000 km2[lower-alpha 2]
Volume 10384000000 km3[lower-alpha 3]
Mass 2.14×1022 kg (0.00359 Earths)[lower-alpha 4]
Mean density
 2.061 g/cm3[5]
0.779 m/s2 (0.0794 g) (0.48 Moons)[lower-alpha 5]
1.455 km/s[lower-alpha 6]
synchronous
5 d, 21 h, 2 min, 53 s[6]
0
Albedo 0.76[5]
Temperature 38 K (−235.2 °C)[6]
13.47[7]
−1.2[8]
Atmosphere
Surface pressure
 1.4–1.9 Pa[6]
(1/70000 the surface pressure on Earth)[9]
Composition by volume nitrogen; methane traces.[10]

Triton is the largest natural satellite of the planet Neptune. It was discovered on October 10, 1846, by English astronomer William Lassell. It is the only large moon in the Solar System with a retrograde orbit, an orbit in the opposite direction to its planet's rotation.[2][11] At 2,700 kilometres (1,700 mi) in diameter, it is the seventh-largest moon in the Solar System. Because of its retrograde orbit and composition similar to Pluto's, Triton is thought to have been a dwarf planet captured from the Kuiper belt.[12] Triton has a surface of mostly frozen nitrogen, a mostly water-ice crust,[13] an icy mantle and a substantial core of rock and metal. The core makes up two-thirds of its total mass. Triton has a mean density of 2.061 g/cm3[5] and is composed of approximately 15–35% water ice.[6]

Triton is one of the few moons in the Solar System known to be geologically active. As a consequence, its surface is relatively young with sparse impact craters, and a complex geological history revealed in intricate cryovolcanic and tectonic terrains. Part of its surface has geysers erupting sublimated nitrogen gas, contributing to a tenuous nitrogen atmosphere less than 1/70,000 the pressure of Earth's atmosphere at sea level.[6]

Discovery and naming

William Lassell, the discoverer of Triton

Triton was discovered by British astronomer William Lassell on October 10, 1846,[14] just 17 days after the discovery of Neptune.

A brewer by trade, Lassell began making mirrors for his amateur telescope in 1820. When John Herschel received news of Neptune's discovery, he wrote to Lassell suggesting he search for possible moons. Lassell did so and discovered Triton eight days later.[15][14] Lassell also claimed to have discovered rings. Although Neptune was later confirmed to have rings, they are so faint and dark that it is doubtful that he actually saw them.[16]

Triton is named after the Greek sea god Triton (Τρίτων), the son of Poseidon (the Greek god comparable to the Roman Neptune). The name was first proposed by Camille Flammarion in his 1880 book Astronomie Populaire,[17] and was officially adopted many decades later.[18] Until the discovery of the second moon Nereid in 1949, Triton was commonly referred to as "the satellite of Neptune". Lassell did not name his own discovery; he later successfully suggested the name Hyperion, previously chosen by John Herschel, for the eighth moon of Saturn when he discovered it.[19]

Orbit and rotation

The orbit of Triton (red) is opposite in direction and tilted −23° compared to a typical moon's orbit (green) in the plane of Neptune's equator.

Triton is unique among all large moons in the Solar System for its retrograde orbit around its planet (i.e. it orbits in a direction opposite to the planet's rotation). Most of the outer irregular moons of Jupiter and Saturn also have retrograde orbits, as do some of Uranus's outer moons. However, these moons are all much more distant from their primaries, and are small in comparison; the largest of them (Phoebe)[lower-alpha 7] has only 8% of the diameter (and 0.03% of the mass) of Triton.

Triton's orbit is associated with two tilts, the inclination of Neptune's spin to Neptune's orbit, 30°, and the inclination of Triton's orbit to Neptune's spin, 157° (an inclination over 90° indicates retrograde motion). Triton's orbit precesses forward relative to Neptune's spin with a period of about 678 Earth years (4.1 Neptunian years),[3][4] making its Neptune-orbit-relative inclination vary between 127° and 180° and in the past, to 173°. That inclination is currently 130°; Triton's orbit is now near its maximum departure from coplanarity with Neptune's.

Triton's rotation is tidally locked to be synchronous with its orbit around Neptune: it keeps one face oriented toward the planet at all times. Its equator is almost exactly aligned with its orbital plane.[20] At the present time, Triton's rotational axis is about 40° from Neptune's orbital plane, and hence at some point during Neptune's year each pole points fairly close to the Sun, almost like the poles of Uranus. As Neptune orbits the Sun, Triton's polar regions take turns facing the Sun, resulting in seasonal changes as one pole, then the other, moves into the sunlight. Such changes were observed in 2010.[21]

Triton's revolution around Neptune has become a nearly perfect circle with an eccentricity of almost zero. Viscoelastic damping from tides alone is not thought to be capable of circularizing Triton's orbit in the time since the origin of the system, and gas drag from a prograde debris disc is likely to have played a substantial role.[3][4] Tidal interactions also cause Triton's orbit, which is already closer to Neptune than the Moon's is to Earth, to gradually decay further; predictions are that 3.6 billion years from now, Triton will pass within Neptune's Roche limit.[22] This will result in either a collision with Neptune's atmosphere or the breakup of Triton, forming a ring system similar to that found around Saturn.[22]

Capture

The Kuiper belt (green), in the Solar System's outskirts, is where Triton is thought to have originated.

Moons in retrograde orbits cannot form in the same region of the solar nebula as the planets they orbit, so Triton must have been captured from elsewhere. It might therefore have originated in the Kuiper belt,[12] a ring of small icy objects extending outwards from just inside the orbit of Neptune to about 50 AU from the Sun. Thought to be the point of origin for the majority of short-period comets observed from Earth, the belt is also home to several large, planet-like bodies including Pluto, which is now recognized as the largest in a population of Kuiper belt objects (the plutinos) locked in orbital step with Neptune. Triton is only slightly larger than Pluto and nearly identical in composition, which has led to the hypothesis that the two share a common origin.[23]

The proposed capture of Triton may explain several features of the Neptunian system, including the extremely eccentric orbit of Neptune's moon Nereid and the scarcity of moons as compared to the other giant planets. Triton's initially eccentric orbit would have intersected orbits of irregular moons and disrupted those of smaller regular moons, dispersing them through gravitational interactions.[3][4]

Triton's eccentric post-capture orbit would have also resulted in tidal heating of its interior, which could have kept Triton fluid for a billion years; this inference is supported by evidence of differentiation in Triton's interior. This source of internal heat disappeared following tidal locking and circularization of the orbit.[24]

Two types of mechanisms have been proposed for Triton's capture. To be gravitationally captured by a planet, a passing body must lose sufficient energy to be slowed down to a speed less than that required to escape. An early theory of how Triton may have been slowed was by collision with another object, either one that happened to be passing by Neptune (which is unlikely), or a moon or proto-moon in orbit around Neptune (which is more likely).[6] A more recent hypothesis suggests that, before its capture, Triton was part of a binary system. When this binary encountered Neptune, it interacted in such a way that the binary dissociated, with one portion of the binary expelled, and the other, Triton, becoming bound to Neptune. This event is more likely for more massive companions.[12] Similar mechanisms have been proposed for the capture of Mars's moons.[25] This hypothesis is supported by several lines of evidence, including binaries being very common among the large Kuiper belt objects.[26][27] The event was brief but gentle, saving Triton from collisional disruption. Events like this may have been common during the formation of Neptune, or later when it migrated outward.[12]

Physical characteristics

Triton dominates the Neptunian moon system, with over 99.5% of its total mass. This imbalance may reflect the elimination of many of Neptune's original satellites following Triton's capture.[3][4]
Triton (lower left) compared to the Moon (upper left) and Earth (right), to scale

Triton is the seventh-largest moon and sixteenth-largest object in the Solar System, and is modestly larger than the dwarf planets Pluto and Eris. It comprises more than 99.5% of all the mass known to orbit Neptune, including the planet's rings and thirteen other known moons,[lower-alpha 8] and is also more massive than all known moons in the Solar System smaller than itself combined.[lower-alpha 9] It has a radius, density (2.061 g/cm3), temperature and chemical composition similar to those of Pluto.[28]

Triton's surface is covered with a transparent layer of annealed frozen nitrogen. Only 40% of Triton's surface has been observed and studied, but it is possible that it is entirely covered in such a thin sheet of nitrogen ice. Like Pluto's, Triton's crust consists of 55% nitrogen ice with other ices mixed in. Water ice comprises 15–35% and frozen carbon dioxide (dry ice) the remaining 10–20%. Trace ices include 0.1% methane and 0.05% carbon monoxide.[6] There could also be ammonia ice on the surface, as there are indications of ammonia dihydrate in the lithosphere.[29] Triton's mean density implies that it probably consists of about 30–45% water ice (including relatively small amounts of volatile ices), with the remainder being rocky material.[6] Triton's surface area is 23 million km2, which is 4.5% of Earth, or 15.5% of Earth's land area. Triton has a considerably and unusually high albedo, reflecting 60–95% of the sunlight that reaches it, and it has changed slightly since the first observations. By comparison, the Moon reflects only 11%.[30] Triton's reddish colour is thought to be the result of methane ice, which is converted to tholins under bombardment from ultraviolet radiation.[6][31]

Because Triton's surface indicates a long history of melting, models of its interior posit that Triton is differentiated, like Earth, into a solid core, a mantle and a crust. Water, the most abundant volatile in the Solar System, comprises Triton's mantle, enveloping a core of rock and metal. There is enough rock in Triton's interior for radioactive decay to power convection in the mantle to this day. The heat may even be sufficient to maintain a global subsurface ocean similar to what is hypothesized to exist beneath the surface of Europa.[6][32] If liquid water is present in Triton, it has been speculated that this could make it habitable for some form of life.[33][34]

Atmosphere

Main article: Atmosphere of Triton
Artist's impression of Triton, showing its tenuous atmosphere just over the limb.

Triton has a tenuous nitrogen atmosphere, with trace amounts of carbon monoxide and small amounts of methane near its surface.[10][35][36] Like Pluto's atmosphere, the atmosphere of Triton is thought to have resulted from evaporation of nitrogen from its surface.[23] Its surface temperature is at least 35.6 K (−237.6 °C) because Triton's nitrogen ice is in the warmer, hexagonal crystalline state, and the phase transition between hexagonal and cubic nitrogen ice occurs at that temperature.[37] An upper limit in the low 40s (K) can be set from vapor pressure equilibrium with nitrogen gas in Triton's atmosphere.[38] This is colder than Pluto's average equilibrium temperature of 44 K (−229 °C). Triton's surface atmospheric pressure is only about 1.4–1.9 Pa (0.014–0.019 mbar).[6]

Clouds observed above Triton's limb by Voyager 2.

Turbulence at Triton's surface creates a troposphere (a "weather region") rising to an altitude of 8 km. Streaks on Triton's surface left by geyser plumes suggest that the troposphere is driven by seasonal winds capable of moving material of over a micrometre in size.[39] Unlike other atmospheres, Triton's lacks a stratosphere, and instead has a thermosphere from altitudes of 8 to 950 km, and an exosphere above that.[6] The temperature of Triton's upper atmosphere, at 95±5 K, is higher than that at its surface, due to heat absorbed from solar radiation and Neptune's magnetosphere.[10][40] A haze permeates most of Triton's troposphere, thought to be composed largely of hydrocarbons and nitriles created by the action of sunlight on methane. Triton's atmosphere also has clouds of condensed nitrogen that lie between 1 and 3 km from its surface.[6]

In 1997, observations from Earth were made of Triton's limb as it passed in front of stars. These observations indicated the presence of a denser atmosphere than was deduced from Voyager 2 data.[41] Other observations have shown an increase in temperature by 5% from 1989 to 1998.[42] These observations indicate Triton is approaching an unusually warm summer season that happens only once every few hundred years. Theories for this warming include a change of frost patterns on Triton's surface and a change in ice albedo, which would allow more heat to be absorbed.[43] Another theory argues the changes in temperature are a result of deposition of dark, red material from geological processes. Because Triton's Bond albedo is among the highest within the Solar System, it is sensitive to small variations in spectral albedo.[44]

Surface features

All detailed knowledge of the surface of Triton was acquired from a distance of 40,000 km by the Voyager 2 spacecraft during a single encounter in 1989.[45] The 40% of Triton's surface imaged by Voyager 2 revealed blocky outcrops, ridges, troughs, furrows, hollows, plateaus, icy plains and few craters. Triton is relatively flat; its observed topography never varies beyond a kilometer.[6] There are relatively few impact craters on Triton. Recent analysis of crater density and distribution has suggested that in geological terms, Triton's surface is extremely young, with regions varying from an estimated 50 million years old to just an estimated 6 million years old.[46]

Cryovolcanism

Main article: Cryovolcano
Dark streaks across Triton's south polar cap surface, thought to be dust deposits left by eruptions of nitrogen geysers

Triton is geologically active; its surface is young and has relatively few impact craters. Although Triton's crust is made of various ices, its subsurface processes are similar to those that produce volcanoes and rift valleys on Earth, but with water and ammonia as opposed to liquid rock.[6] Triton's entire surface is cut by complex valleys and ridges, probably the result of tectonics and icy volcanism. The vast majority of surface features on Triton are endogenic—the result of internal geological processes rather than external processes such as impacts. Most are volcanic and extrusive in nature, rather than tectonic.[6]

The Voyager 2 probe observed a handful of geyser-like eruptions of invisible nitrogen gas and entrained dust from beneath the surface of Triton in plumes up to 8 km high.[28][47] Triton is thus, along with Earth, Io, and Enceladus, one of the few bodies in the Solar System on which active eruptions of some sort have been observed.[48] The best-observed examples were named Hili and Mahilani (after a Zulu water sprite and a Tongan sea spirit, respectively).[49]

All the geysers observed were located between 50° and 57°S, the part of Triton's surface close to the subsolar point. This indicates that solar heating, although very weak at Triton's great distance from the Sun, plays a crucial role. It is thought that the surface of Triton probably consists of a translucent layer of frozen nitrogen overlying a darker substrate, which creates a kind of "solid greenhouse effect". Solar radiation passes through the thin surface ice sheet, slowly heating and vaporizing subsurface nitrogen until enough gas pressure accumulates for it to erupt through the crust.[6][39] A temperature increase of just 4 K above the ambient surface temperature of 37 K could drive eruptions to the heights observed.[47] Although commonly termed "cryovolcanic", this nitrogen plume activity is distinct from Triton's larger scale cryovolcanic eruptions, as well as volcanic processes on other worlds, which are powered by the internal heat of the body in question. Analogous CO2 geysers on Mars are thought to erupt from its south polar cap each spring.[50]

Each eruption of a Triton geyser may last up to a year, driven by the sublimation of about 100 million cubic metres (3.5×10^9 cu ft) of nitrogen ice over this interval; dust entrained may be deposited up to 150 km downwind in visible streaks, and perhaps much farther in more diffuse deposits.[47] Voyager 2's images of Triton's southern hemisphere show many such streaks of dark material.[51] Between 1977 and the Voyager 2 flyby in 1989, Triton shifted from a reddish colour, similar to Pluto, to a far paler hue, suggesting that lighter nitrogen frosts had covered older reddish material.[6] The eruption of volatiles from Triton's equator and their deposition at the poles may redistribute enough mass over the course of 10,000 years to cause polar wander.[52]

Polar cap, plains and ridges

Triton's bright south polar cap above a region of cantaloupe terrain

Triton's south polar region is covered by a highly reflective cap of frozen nitrogen and methane sprinkled by impact craters and openings of geysers. Little is known about the north pole because it was on the night side during the Voyager 2 encounter, but it is thought that Triton must also have a north polar ice cap.[37]

The high plains found on Triton's eastern hemisphere, such as Cipango Planum, cover over and blot out older features, and are therefore almost certainly the result of icy lava washing over the previous landscape. The plains are dotted with pits, such as Leviathan Patera, which are probably the vents from which this lava emerged. The composition of the lava is unknown, although a mixture of ammonia and water is suspected.[6]

Four roughly circular "walled plains" have been identified on Triton. They are the flattest regions so far discovered, with a variance in altitude of less than 200 m. They are thought to have formed from eruption of icy lava.[6] The plains near Triton's eastern limb are dotted with black spots, the maculae. Some maculae are simple dark spots with diffuse boundaries, and other comprise a dark central patch surrounded by a white halo with sharp boundaries. Typical diameter of maculae is about 100 km and width of halo is between 20 and 30 km. Some speculate the maculae are outliers of the south polar cap, which retreats in summer.[6]

There are extensive ridges and valleys in complex patterns across Triton's surface, probably the result of freeze–thaw cycles.[53] Many also appear to be tectonic in nature and may result from extension or strike-slip faulting.[54] There are long double ridges of ice with central troughs bearing a strong resemblance to Europan lineae (although they have a larger scale[13]), and which may have a similar origin,[6] possibly shear heating from strike-slip motion along faults caused by diurnal tidal stresses experienced before Triton's orbit was fully circularized.[13] These faults with parallel ridges expelled from the interior cross complex terrain with valleys in the equatorial region. The ridges and furrows, or sulci, such as Yasu Sulci, Ho Sulci, and Lo Sulci,[55] are thought to be of intermediate age in Triton's geological history, and in many cases to have formed concurrently. They tend to be clustered in groups or "packets".[54]

Cantaloupe terrain

Cantaloupe terrain viewed from 130,000 km by Voyager 2, with crosscutting Europa-like double ridges. Slidr Sulci (vertical) and Tano Sulci form the prominent "X".

Triton's western hemisphere consists of a strange series of fissures and depressions known as "cantaloupe terrain" because of its resemblance to the skin of a cantaloupe melon. Although it has few craters, it is thought that this is the oldest terrain on Triton.[56] It probably covers much of Triton's western half.[6]

Cantaloupe terrain, which is mostly dirty water ice, is known to exist only on Triton. It contains depressions 30–40 km in diameter.[56] The depressions (cavi) are probably not impact craters because they are all of similar size and have smooth curves. The leading hypothesis for their formation is diapirism, the rising of "lumps" of less dense material through a stratum of denser material.[6][57] Alternative hypotheses include formation by collapses, or by flooding caused by cryovolcanism.[56]

Impact craters

Tuonela Planitia (left) and Ruach Planitia (center) are two of Triton's cryovolcanic "walled plains". The paucity of craters is evidence of extensive geologic activity.

Due to constant erasure and modification by ongoing geological activity, impact craters on Triton's surface are relatively rare. A census of Triton's craters imaged by Voyager 2 found only 179 that were incontestably of impact origin, compared with 835 observed for Uranus's moon Miranda, which has only three percent of Triton's surface area.[58] The largest crater observed on Triton thought to have been created by an impact is a 27 km-diameter feature called Mazomba.[58][59] Although larger craters have been observed, they are generally thought to be volcanic in nature.[58]

The few impact craters on Triton are almost all concentrated in the leading hemisphere—that facing the direction of the orbital motion—with the majority concentrated around the equator between 30° and 70° longitude,[58] resulting from material swept up from orbit around Neptune.[46] Because it orbits with one side permanently facing the planet, astronomers expect that Triton should have fewer impacts on its trailing hemisphere, due to impacts on the leading hemisphere being more frequent and more violent.[58] Voyager 2 imaged only 40% of Triton's surface, so this remains uncertain.

Observation and exploration

Neptune (top) and Triton (bottom) three days after Voyager 2's flyby

The orbital properties of Triton were already determined with high accuracy in the 19th century. It was found to have a retrograde orbit, at a very high angle of inclination to the plane of Neptune's orbit. The first detailed observations of Triton were not made until 1930. Little was known about the satellite until Voyager 2 arrived at the end of the 20th century.[6]

Before the arrival of Voyager 2, astronomers suspected that Triton might have liquid nitrogen seas and a nitrogen/methane atmosphere with a density as much as 30% that of Earth. Like the famous overestimates of the atmospheric density of Mars, this proved completely false. As with Mars, a denser atmosphere is postulated for its early history.[60]

The first attempt to measure the diameter of Triton was made by Gerard Kuiper in 1954. He obtained a value of 3,800 km. Subsequent measurement attempts arrived at values ranging from 2,500 to 6,000 km, or from slightly smaller than the Moon (3474.2 km) to nearly half the diameter of Earth.[61] Data from the approach of Voyager 2 to Neptune on August 25, 1989, led to a more accurate estimate of Triton's diameter (2,706 km).[62]

In the 1990s, various observations from Earth were made of the limb of Triton using the occultation of nearby stars, which indicated the presence of an atmosphere and an exotic surface. The observations suggest that the atmosphere is denser than the Voyager 2 measurements had indicated.[41]

New concepts for missions to the Neptune system to be conducted in the 2010s have been brought forward by NASA scientists on numerous occasions over the last decades. All of them identified Triton as being a prime target and a separate Triton lander comparable to the Huygens probe for Titan was frequently included in those plans. No efforts aimed at Neptune and Triton went beyond the proposal phase and NASA's funding on missions to the outer Solar System is currently focused on the Jupiter and Saturn systems.[63]

A proposed lander mission to Triton, called Triton Hopper, would mine and process nitrogen ice from the surface of Triton and process it to be used as small rocket propellant and fly or 'hop' across the surface.[64]

Maps

Enhanced-color map; leading hemisphere is on right
Enhanced-color polar maps; south is right

See also

Notes

  1. ↑ Photomosaic of Triton's sub-Neptunian hemisphere. The bright, slightly pinkish, south polar cap at bottom is composed of nitrogen and methane ice and is streaked by dust deposits left by nitrogen gas geysers. The mostly darker region above it includes Triton's "cantaloupe terrain" and cryovolcanic and tectonic features. Near the lower right limb are several dark maculae ("strange spots").
  1. ↑ Calculated on the basis of other parameters.
  2. ↑ Surface area derived from the radius r: 4×π×r2.
  3. ↑ Volume v derived from the radius r: 4⁄3×π×r3.
  4. ↑ Mass m derived from the density d and the volume v: m=d×v.
  5. ↑ Surface gravity derived from the mass m, the gravitational constant g and the radius r: g×m/r2 .
  6. ↑ Escape velocity derived from the mass m, the gravitational constant g and the radius r: √(̅2̅×̅g̅×̅m̅)̅/̅r̅.
  7. ↑ Largest irregular moons: Saturn's Phoebe (210 km), Uranus's Sycorax (150 km), and Jupiter's Himalia (85 km)
  8. ↑ 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.
  9. ↑ The masses of other spherical moons are: Titania—3.5×1021, Oberon—3.0×1021, Rhea—2.3×1021, Iapetus—1.8×1021, Charon—1.5×1021, Ariel—1.3×1021, Umbriel—1.2×1021, Dione—1.0×1021, Tethys—0.6×1021, Enceladus—0.12×1021, Miranda—0.06×1021, Proteus—0.05×1021, Mimas—0.04×1021. The total mass of remaining moons is about 0.09×1021. So, the total mass of all moons smaller than Triton is about 1.65×1022. (See List of moons by diameter)

References

  1. 1 2 Williams, David R. (November 23, 2006). "Neptunian Satellite Fact Sheet". NASA. Archived from the original on October 5, 2011. Retrieved January 18, 2008.
  2. 1 2 Overbye, Dennis (November 5, 2014). "Bound for Pluto, Carrying Memories of Triton". New York Times. Retrieved November 5, 2014.
  3. 1 2 3 4 5 Jacobson, R. A. — AJ (April 3, 2009). "Planetary Satellite Mean Orbital Parameters". JPL satellite ephemeris. JPL (Solar System Dynamics). Retrieved October 26, 2011. Archived October 5, 2011, at WebCite
  4. 1 2 3 4 5 Jacobson, R. A. (3 April 2009). "The Orbits of the Neptunian Satellites and the Orientation of the Pole of Neptune". The Astronomical Journal. 137 (5): 4322–4329. Bibcode:2009AJ....137.4322J. doi:10.1088/0004-6256/137/5/4322.
  5. 1 2 3 4 "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). Archived from the original on January 18, 2010. Retrieved October 26, 2011.
  6. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 McKinnon, William B.; Kirk, Randolph L. (2014). "Triton". In Tilman Spohn; Doris Breuer; Torrence Johnson. Encyclopedia of the Solar System (3rd ed.). Amsterdam; Boston: Elsevier. pp. 861–882. ISBN 978-0-12-416034-7.
  7. ↑ "Classic Satellites of the Solar System". Observatorio ARVAL. Archived from the original on August 25, 2011. Retrieved September 28, 2007.
  8. ↑ Fischer, Daniel (February 12, 2006). "Kuiperoids & Scattered Objects". Argelander-Institut für Astronomie. Archived from the original on October 5, 2011. Retrieved July 1, 2008.
  9. ↑ "Neptune: Moons: Triton". NASA. Archived from the original on October 5, 2011. Retrieved September 21, 2007.
  10. 1 2 3 Broadfoot, A. L.; Atreya, S. K.; Bertaux, J. L.; Blamont, J. E.; Dessler, A. J.; Donahue, T. M.; Forrester, W. T.; Hall, D. T.; Herbert, F.; Holberg, J. B.; Hunter, D. M.; Krasnopolsky, V. A.; Linick, S.; Lunine, J. I.; McConnell, J. C.; Moos, H. W.; Sandel, B. R.; Schneider, N. M.; Shemansky, D. E.; Smith, G. R.; Strobel, D. F.; Yelle, R. V. (1989). "Ultraviolet Spectrometer Observations of Neptune and Triton". Science. 246 (4936): 1459–66. Bibcode:1989Sci...246.1459B. doi:10.1126/science.246.4936.1459. PMID 17756000.
  11. ↑ Chang, Kenneth (18 October 2014). "Dark Spots in Our Knowledge of Neptune". New York Times. Retrieved 21 October 2014.
  12. 1 2 3 4 Agnor, C. B.; Hamilton, D. P. (2006). "Neptune's capture of its moon Triton in a binary–planet gravitational encounter" (PDF). Nature. 441 (7090): 192–4. Bibcode:2006Natur.441..192A. doi:10.1038/nature04792. PMID 16688170.
  13. 1 2 3 Prockter, L. M.; Nimmo, F.; Pappalardo, R. T. (July 30, 2005). "A shear heating origin for ridges on Triton" (PDF). Geophysical Research Letters. 32 (14): L14202. Bibcode:2005GeoRL..3214202P. doi:10.1029/2005GL022832. Retrieved October 9, 2011.
  14. 1 2 Lassell, William (November 12, 1847). "Lassell's Satellite of Neptune". Monthly Notices of the Royal Astronomical Society. 8 (1): 8. Bibcode:1847MNRAS...8....9B. doi:10.1093/mnras/10.1.8.
  15. ↑ Lassell, William (November 13, 1846). "Discovery of Supposed Ring and Satellite of Neptune". Monthly Notices of the Royal Astronomical Society. 7 (9): 157. Bibcode:1846MNRAS...7..157L. doi:10.1093/mnras/7.9.154.
    Lassell, William (December 11, 1846). "Physical observations on Neptune". Monthly Notices of the Royal Astronomical Society. 7 (10): 167–168. Bibcode:1847MNRAS...7..297L. doi:10.1093/mnras/7.10.165a.
    Lassell, W. (1847). "Observations of Neptune and his satellite". Monthly Notices of the Royal Astronomical Society. 7 (17): 307–308. Bibcode:1847MNRAS...7..307L. doi:10.1002/asna.18530360703.
  16. ↑ Smith, R. W.; Baum, R. (1984). "William Lassell and the Ring of Neptune: A Case Study in Instrumental Failure". Journal of the History of Astronomy. 15 (42): 1–17. Bibcode:1984JHA....15....1S.
  17. ↑ Flammarion, Camille (1880). "Astronomie populaire". p. 591. Archived from the original on October 5, 2011. Retrieved April 10, 2007.
  18. ↑ Moore, Patrick (April 1996). The planet Neptune: an historical survey before Voyager. Wiley-Praxis Series in Astronomy and Astrophysics (2nd ed.). John Wiley & Sons. pp. 150 (see p. 68). ISBN 978-0-471-96015-7. OCLC 33103787.
  19. ↑ "Planet and Satellite Names and their Discoverers". International Astronomical Union. Archived from the original on February 12, 2008. Retrieved January 13, 2008.
  20. ↑ Davies, M.; Rogers, P.; Colvin, T. (1991). "A Control Network of Triton" (PDF). J. Geophys. Res. 96(E1): 15675–15681. Bibcode:1991JGR....9615675D. doi:10.1029/91JE00976.
  21. ↑ Seasons Discovered on Neptune's Moon Triton — Space.com (2010) Archived October 5, 2011, at WebCite
  22. 1 2 Chyba, C. F.; Jankowski, D. G.; Nicholson, P. D. (July 1989). "Tidal evolution in the Neptune-Triton system". Astronomy and Astrophysics. 219 (1–2): L23–L26. Bibcode:1989A&A...219L..23C.
  23. 1 2 Cruikshank, Dale P. (2004). "Triton, Pluto, Centaurs, and Trans-Neptunian Bodies". Space Science Reviews. 116: 421–439. Bibcode:2005SSRv..116..421C. doi:10.1007/s11214-005-1964-0. ISBN 978-1-4020-3362-9.
  24. ↑ Ross, MN; Schubert, G (September 1990). "The coupled orbital and thermal evolution of Triton". Geophysical Research Letters. 17 (10): 1749–1752. doi:10.1029/GL017i010p01749.
  25. ↑ "Origin of Martian Moons from Binary Asteroid Dissociation", AAAS – 57725, American Association for Advancement of Science Annual Meeting 2002
  26. ↑ EXTREME KUIPER BELT OBJECT 2001QG298 AND THE FRACTION OF CONTACT BINARIES Archived October 5, 2011, at WebCite
  27. ↑ Jewitt, Dave (2005). "Binary Kuiper Belt Objects". University of Hawaii. Archived from the original on October 5, 2011. Retrieved June 24, 2007.
  28. 1 2 "Triton (Voyager)". NASA. June 1, 2005. Archived from the original on October 5, 2011. Retrieved December 9, 2007.
  29. ↑ Ruiz, Javier (December 2003). "Heat flow and depth to a possible internal ocean on Triton". Icarus. 166 (2): 436–439. Bibcode:2003Icar..166..436R. doi:10.1016/j.icarus.2003.09.009.
  30. ↑ Medkeff, Jeff (2002). "Lunar Albedo". Sky and Telescope Magazine. Archived from the original on May 23, 2008. Retrieved February 4, 2008.
  31. ↑ Grundy, W. M.; Buie, M. W.; Spencer, J. R. (October 2002). "Spectroscopy of Pluto and Triton at 3–4 Microns: Possible Evidence for Wide Distribution of Nonvolatile Solids". The Astronomical Journal. 124 (4): 2273–2278. Bibcode:2002AJ....124.2273G. doi:10.1086/342933.
  32. ↑ Hussmann, Hauke; Sohl, Frank; Spohn, Tilman (November 2006). "Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects" (PDF). Icarus. 185 (1): 258–273. Bibcode:2006Icar..185..258H. doi:10.1016/j.icarus.2006.06.005.
  33. ↑ Irwin, L. N.; Schulze-Makuch, D. (2001). "Assessing the Plausibility of Life on Other Worlds". Astrobiology. 1 (2): 143–60. Bibcode:2001AsBio...1..143I. doi:10.1089/153110701753198918. PMID 12467118.
  34. ↑ Doyle, Amanda (September 6, 2012). "Does Neptune's moon Triton have a subsurface ocean?". Space.com. Retrieved September 18, 2015.
  35. ↑ Miller, Ron; Hartmann, William K. (May 2005). The Grand Tour: A Traveler's Guide to the Solar System (3rd ed.). Thailand: Workman Publishing. pp. 172–73. ISBN 978-0-7611-3547-0.
  36. ↑ Lellouch, E.; de Bergh, C.; Sicardy, B.; Ferron, S.; Käufl, H.-U. (2010). "Detection of CO in Triton's atmosphere and the nature of surface-atmosphere interactions". Astronomy & Astrophysics. 512: L8. arXiv:1003.2866Freely accessible. Bibcode:2010A&A...512L...8L. doi:10.1051/0004-6361/201014339.
  37. 1 2 Duxbury, N S; Brown, R H (August 1993). "The Phase Composition of Triton's Polar Caps". Science. 261 (5122): 748–751. Bibcode:1993Sci...261..748D. doi:10.1126/science.261.5122.748. PMID 17757213.
  38. ↑ Tryka, K. A.; Brown, R. H.; Anicich, V.; Cruikshank, D. P.; Owen, T. C. (1993). "Spectroscopic Determination of the Phase Composition and Temperature of Nitrogen Ice on Triton". Science. 261 (5122): 751–4. Bibcode:1993Sci...261..751T. doi:10.1126/science.261.5122.751. PMID 17757214.
  39. 1 2 Smith, B. A.; Soderblom, L. A.; Banfield, D.; Barnet, C.; Basilevsky, A. T.; Beebe, R. F.; Bollinger, K.; Boyce, J. M.; Brahic, A. (1989). "Voyager 2 at Neptune: Imaging Science Results". Science. 246 (4936): 1422–1449. Bibcode:1989Sci...246.1422S. doi:10.1126/science.246.4936.1422. PMID 17755997.
  40. ↑ Stevens, M. H.; Strobel, D. F.; Summers, M. E.; Yelle, R. V. (April 3, 1992). "On the thermal structure of Triton's thermosphere". Geophysical Research Letters. 19 (7): 669–672. Bibcode:1992GeoRL..19..669S. doi:10.1029/92GL00651. Retrieved October 8, 2011.
  41. 1 2 Savage, D.; Weaver, D.; Halber, D. (June 24, 1998). "Hubble Space Telescope Helps Find Evidence that Neptune's Largest Moon Is Warming Up". Hubblesite. STScI-1998-23. Archived from the original on October 5, 2011. Retrieved December 31, 2007.
  42. ↑ "MIT researcher finds evidence of global warming on Neptune's largest moon". Massachusetts Institute of Technology. June 24, 1998. Archived from the original on October 5, 2011. Retrieved December 31, 2007.
  43. ↑ MacGrath, Melissa (June 28, 1998). "Solar System Satellites and Summary". Hubble's Science Legacy: Future Optical/Ultraviolet Astronomy from Space. Space Telescope Science Institute. 291: 93. Bibcode:2003ASPC..291...93M.
  44. ↑ Buratti, Bonnie J.; Hicks, Michael D.; Newburn, Ray L. Jr. (January 21, 1999). "Does global warming make Triton blush?" (PDF). Nature. 397 (6716): 219–20. Bibcode:1999Natur.397..219B. doi:10.1038/16615. PMID 9930696. Retrieved December 31, 2007.
  45. ↑ Gray, D (1989). "Voyager 2 Neptune navigation results". Astrodynamics Conference: 108. doi:10.2514/6.1990-2876.
  46. 1 2 Schenk, Paul M.; Zahnle, Kevin (December 2007). "On the negligible surface age of Triton". Icarus. 192 (1): 135–49. Bibcode:2007Icar..192..135S. doi:10.1016/j.icarus.2007.07.004.
  47. 1 2 3 Soderblom, L. A.; Kieffer, S. W.; Becker, T. L.; Brown, R. H.; Cook, A. F. II; Hansen, C. J.; Johnson, T. V.; Kirk, R. L.; Shoemaker, E. M. (October 19, 1990). "Triton's Geyser-Like Plumes: Discovery and Basic Characterization". Science. 250 (4979): 410–415. Bibcode:1990Sci...250..410S. doi:10.1126/science.250.4979.410. PMID 17793016.
  48. ↑ Kargel, JS (1994). "Cryovolcanism on the icy satellites". Earth, Moon, and Planets (published 1995). 67 (1–3): 101–113. Bibcode:1995EM&P...67..101K. doi:10.1007/BF00613296.
  49. ↑ USGS Astrogeology Research Program: Gazetteer of Planetary Nomenclature, search for "Hili" and "Mahilani" Archived October 5, 2011, at WebCite
  50. ↑ Burnham, Robert (August 16, 2006). "Gas jet plumes unveil mystery of 'spiders' on Mars". Arizona State University. Archived from the original on October 5, 2011. Retrieved August 29, 2009.
  51. ↑ Kirk, R. L. (1990). "Thermal Models of Insolation-Driven Nitrogen Geysers on Triton". LPSC XXI. Lunar and Planetary Institute. pp. 633–634. Bibcode:1990LPI....21..633K.
  52. ↑ Rubincam, David Parry (2002). "Polar wander on Triton and Pluto due to volatile migration". Icarus. 163 (2): 63–71. Bibcode:2003Icar..163..469R. doi:10.1016/S0019-1035(03)00080-0.
  53. ↑ Elliot, J. L.; Hammel, H. B.; Wasserman, L. H.; Franz, O. G.; McDonald, S. W.; Person, M. J.; Olkin, C. B.; Dunham, E. W.; Spencer, J. R.; Stansberry, J. A.; Buie, M. W.; Pasachoff, J. M.; Babcock, B. A.; McConnochie, T. H. (1998). "Global warming on Triton". Nature. 393 (6687): 765–767. Bibcode:1998Natur.393..765E. doi:10.1038/31651.
  54. 1 2 Collins, Geoffrey; Schenk, Paul (March 14–18, 1994). "Triton's Lineaments: Complex Morphology and Stress Patterns". Abstracts of the 25th Lunar and Planetary Science Conference. Houston, TX. 25: 277. Bibcode:1994LPI....25..277C.
  55. ↑ Aksnes, K; Brahic, A; Fulchignoni, M; Marov, M Ya (1990). "Working Group for Planetary System Nomenclature" (PDF). Reports on Astronomy. State University of New York (published 1991). 21A: 613–19. 1991IAUTA..21..613A. Retrieved January 25, 2008.
  56. 1 2 3 Boyce, Joseph M. (March 1993). "A structural origin for the cantaloupe terrain of Triton". In Lunar and Planetary Inst., Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F (SEE N94-12015 01-91). 24: 165–66. Bibcode:1993LPI....24..165B.
  57. ↑ Schenk, P.; Jackson, M. P. A. (April 1993). "Diapirism on Triton: A record of crustal layering and instability". Geology. 21 (4): 299–302. Bibcode:1993Geo....21..299S. doi:10.1130/0091-7613(1993)021<0299:DOTARO>2.3.CO;2.
  58. 1 2 3 4 5 Strom, Robert G.; Croft, Steven K.; Boyce, Joseph M. (1990). "The Impact Cratering Record on Triton". Science. 250 (4979): 437–39. Bibcode:1990Sci...250..437S. doi:10.1126/science.250.4979.437. PMID 17793023.
  59. ↑ Ingersoll, Andrew P.; Tryka, Kimberly A. (1990). "Triton's Plumes: The Dust Devil Hypothesis". Science. 250 (4979): 435–437. Bibcode:1990Sci...250..435I. doi:10.1126/science.250.4979.435. PMID 17793022.
  60. ↑ Lunine, Jonathan I.; Nolan, Michael C. (November 1992). "A massive early atmosphere on Triton". Icarus. 100 (1): 221–34. Bibcode:1992Icar..100..221L. doi:10.1016/0019-1035(92)90031-2.
  61. ↑ Cruikshank, D. P.; Stockton, A.; Dyck, H. M.; Becklin, E. E.; Macy, W. (1979). "The diameter and reflectance of Triton". Icarus. 40: 104–114. Bibcode:1979Icar...40..104C. doi:10.1016/0019-1035(79)90057-5.
  62. ↑ Stone, EC; Miner, ED (December 15, 1989). "The Voyager 2 Encounter with the Neptunian System". Science. 246 (4936): 1417–21. Bibcode:1989Sci...246.1417S. doi:10.1126/science.246.4936.1417. PMID 17755996. And the following 12 articles pp. 1422–1501.
  63. ↑ "USA.gov: The U.S. Government's Official Web Portal" (PDF). Nasa.gov. September 27, 2013. Retrieved 2013-10-10.
  64. ↑ Becky Ferreira, Why We Should Use This Jumping Robot to Explore Neptune, Motherboard, August 28, 2015 // 08:00 AM EST (Retrieved September 14, 2014)

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