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Jupiter trojan

The Jupiter trojans, commonly called trojan asteroids or simply trojans, are a large group of asteroids that share the planet Jupiter's orbit around the Sun. Relative to Jupiter, each trojan librates around one of Jupiter's stable Lagrange points: either L4, existing 60° ahead of the planet in its orbit, or L5, 60° behind. Jupiter trojans are distributed in two elongated, curved regions around these Lagrangian points with an average semi-major axis of about 5.2 AU.[1]

The asteroids of the inner Solar System and Jupiter
  Jupiter trojans
  Hilda asteroids
  Asteroid belt
  Orbits of planets
The Jupiter trojans are divided into two groups: The Greek camp in front of and the Trojan camp trailing behind Jupiter in their orbit.

The first Jupiter trojan discovered, 588 Achilles, was spotted in 1906 by German astronomer Max Wolf.[2] More than 9,800 Jupiter trojans have been found as of May 2021.[3] By convention, they are each named from Greek mythology after a figure of the Trojan War, hence the name "trojan". The total number of Jupiter trojans larger than 1 km in diameter is believed to be about 1 million,[1] approximately equal to the number of asteroids larger than 1 km in the asteroid belt.[4] Like main-belt asteroids, Jupiter trojans form families.[5]

As of 2004, many Jupiter trojans showed to observational instruments as dark bodies with reddish, featureless spectra. No firm evidence of the presence of water, or any other specific compound on their surface has been obtained, but it is thought that they are coated in tholins, organic polymers formed by the Sun's radiation.[6] The Jupiter trojans' densities (as measured by studying binaries or rotational lightcurves) vary from 0.8 to 2.5 g·cm−3.[5] Jupiter trojans are thought to have been captured into their orbits during the early stages of the Solar System's formation or slightly later, during the migration of giant planets.[5]

The term "Trojan Asteroid" specifically refers to the asteroids co-orbital with Jupiter, but the general term "trojan" is sometimes more generally applied to other small Solar System bodies with similar relationships to larger bodies: Mars trojans, Neptune trojans, Uranus trojans and Earth trojans are known to exist.[7] [8][9] The term "Trojan asteroid" is normally understood to specifically mean the Jupiter trojans because the first Trojans were discovered near Jupiter's orbit and Jupiter currently has by far the most known Trojans.[3]

Observational history

 
Maximilian Franz Joseph Cornelius Wolf (1890)—the discoverer of the first trojan

In 1772, Italian-born mathematician Joseph-Louis Lagrange, in studying the restricted three-body problem, predicted that a small body sharing an orbit with a planet but lying 60° ahead or behind it will be trapped near these points.[2] The trapped body will librate slowly around the point of equilibrium in a tadpole or horseshoe orbit.[10] These leading and trailing points are called the L4 and L5 Lagrange points.[11][Note 1] The first asteroids trapped in Lagrange points were observed more than a century after Lagrange's hypothesis. Those associated with Jupiter were the first to be discovered.[2]

E. E. Barnard made the first recorded observation of a trojan, (12126) 1999 RM11 (identified as A904 RD at the time), in 1904, but neither he nor others appreciated its significance at the time.[12] Barnard believed he had seen the recently discovered Saturnian satellite Phoebe, which was only two arc-minutes away in the sky at the time, or possibly an asteroid. The object's identity was not understood until its orbit was calculated in 1999.[12]

The first accepted discovery of a trojan occurred in February 1906, when astronomer Max Wolf of Heidelberg-Königstuhl State Observatory discovered an asteroid at the L4 Lagrangian point of the SunJupiter system, later named 588 Achilles.[2] In 1906–1907 two more Jupiter trojans were found by fellow German astronomer August Kopff (624 Hektor and 617 Patroclus).[2] Hektor, like Achilles, belonged to the L4 swarm ("ahead" of the planet in its orbit), whereas Patroclus was the first asteroid known to reside at the L5 Lagrangian point ("behind" the planet).[13] By 1938, 11 Jupiter trojans had been detected.[14] This number increased to 14 only in 1961.[2] As instruments improved, the rate of discovery grew rapidly: by January 2000, a total of 257 had been discovered;[11] by May 2003, the number had grown to 1,600.[15] As of October 2018 there are 4,601 known Jupiter trojans at L4 and 2,439 at L5.[16]

Nomenclature

The custom of naming all asteroids in Jupiter's L4 and L5 points after famous heroes of the Trojan War was suggested by Johann Palisa of Vienna, who was the first to accurately calculate their orbits.[2]

Asteroids in the leading (L4) orbit are named after Greek heroes (the "Greek node or camp" or "Achilles group"), and those at the trailing (L5) orbit are named after the heroes of Troy (the "Trojan node or camp").[2] The asteroids 617 Patroclus and 624 Hektor were named before the Greece/Troy rule was devised, resulting in a "Greek spy", Patroclus, in the Trojan node and a "Trojan spy", Hector, in the Greek node.[14][17]

Numbers and mass

 
A gravitational potential contour plot showing Earth's Lagrangian points; L4 and L5 are ahead (above) and behind (below) the planet, respectively. Jupiter's Lagrangian points are similarly situated in its much larger orbit.

Estimates of the total number of Jupiter trojans are based on deep surveys of limited areas of the sky.[1] The L4 swarm is believed to hold between 160,000 and 240,000 asteroids with diameters larger than 2 km and about 600,000 with diameters larger than 1 km.[1][11] If the L5 swarm contains a comparable number of objects, there are more than 1 million Jupiter trojans 1 km in size or larger. For the objects brighter than absolute magnitude 9.0 the population is probably complete.[15] These numbers are similar to that of comparable asteroids in the asteroid belt.[1] The total mass of the Jupiter trojans is estimated at 0.0001 of the mass of Earth or one-fifth of the mass of the asteroid belt.[11]

Two more recent studies indicate that the above numbers may overestimate the number of Jupiter trojans by several-fold. This overestimate is caused by (1) the assumption that all Jupiter trojans have a low albedo of about 0.04, whereas small bodies may have an average albedo as high as 0.12;[18] (2) an incorrect assumption about the distribution of Jupiter trojans in the sky.[19] According to the new estimates, the total number of Jupiter trojans with a diameter larger than 2 km is 6,300 ± 1,000 and 3,400 ± 500 in the L4 and L5 swarms, respectively.[19] These numbers would be reduced by a factor of 2 if small Jupiter trojans are more reflective than large ones.[18]

The number of Jupiter trojans observed in the L4 swarm is slightly larger than that observed in L5. Because the brightest Jupiter trojans show little variation in numbers between the two populations, this disparity is probably due to observational bias.[5] Some models indicate that the L4 swarm may be slightly more stable than the L5 swarm.[10]

The largest Jupiter trojan is 624 Hektor, which has a mean diameter of 203 ± 3.6 km.[15] There are few large Jupiter trojans in comparison to the overall population. With decreasing size, the number of Jupiter trojans grows very quickly down to 84 km, much more so than in the asteroid belt. A diameter of 84 km corresponds to an absolute magnitude of 9.5, assuming an albedo of 0.04. Within the 4.4–40 km range the Jupiter trojans' size distribution resembles that of the main-belt asteroids. Nothing is known about the masses of the smaller Jupiter trojans.[10] The size distribution suggests that the smaller Trojans may be the products of collisions by larger Jupiter trojans.[5]

The largest Jupiter trojans
Trojan Diameter (km)
624 Hektor 225
617 Patroclus 140
911 Agamemnon 131
588 Achilles 130
3451 Mentor 126
3317 Paris 119
1867 Deiphobus 118
1172 Äneas 118
1437 Diomedes 118
1143 Odysseus 115
Source: JPL Small-Body Database, NEOWISE data

Orbits

 
Animation of the orbit of 624 Hektor (blue), set against the orbit of Jupiter (outer red ellipse)

Jupiter trojans have orbits with radii between 5.05 and 5.35 AU (the mean semi-major axis is 5.2 ± 0.15 AU), and are distributed throughout elongated, curved regions around the two Lagrangian points;[1] each swarm stretches for about 26° along the orbit of Jupiter, amounting to a total distance of about 2.5 AU.[11] The width of the swarms approximately equals two Hill's radii, which in the case of Jupiter amounts to about 0.6 AU.[10] Many of Jupiter trojans have large orbital inclinations relative to Jupiter's orbital plane—up to 40°.[11]

Jupiter trojans do not maintain a fixed separation from Jupiter. They slowly librate around their respective equilibrium points, periodically moving closer to Jupiter or farther from it.[10] Jupiter trojans generally follow paths called tadpole orbits around the Lagrangian points; the average period of their libration is about 150 years.[11] The amplitude of the libration (along the Jovian orbit) varies from 0.6° to 88°, with the average being about 33°.[10] Simulations show that Jupiter trojans can follow even more complicated trajectories when moving from one Lagrangian point to another—these are called horseshoe orbits (currently no Jupiter Trojan with such an orbit is known, though one is known for Neptune).[10]

Dynamical families and binaries

Discerning dynamical families within the Jupiter trojan population is more difficult than it is in the asteroid belt, because the Jupiter trojans are locked within a far narrower range of possible positions. This means that clusters tend to overlap and merge with the overall swarm. By 2003 roughly a dozen dynamical families were identified. Jupiter-trojan families are much smaller in size than families in the asteroid belt; the largest identified family, the Menelaus group, consists of only eight members.[5]

In 2001, 617 Patroclus was the first Jupiter trojan to be identified as a binary asteroid.[20] The binary's orbit is extremely close, at 650 km, compared to 35,000 km for the primary's Hill sphere.[21] The largest Jupiter trojan—624 Hektor— is probably a contact binary with a moonlet.[5][22][23]

Physical properties

 
Trojan 624 Hektor (indicated) is similar in brightness to dwarf planet Pluto.

Jupiter trojans are dark bodies of irregular shape. Their geometric albedos generally vary between 3 and 10%.[15] The average value is 0.056 ± 0.003 for the objects larger than 57 km,[5] and 0.121 ± 0.003 (R-band) for those smaller than 25 km.[18] The asteroid 4709 Ennomos has the highest albedo (0.18) of all known Jupiter trojans.[15] Little is known about the masses, chemical composition, rotation or other physical properties of the Jupiter trojans.[5]

Rotation

The rotational properties of Jupiter trojans are not well known. Analysis of the rotational light curves of 72 Jupiter trojans gave an average rotational period of about 11.2 hours, whereas the average period of the control sample of asteroids in the asteroid belt was 10.6 hours.[24] The distribution of the rotational periods of Jupiter trojans appeared to be well approximated by a Maxwellian function,[Note 2] whereas the distribution for main-belt asteroids was found to be non-Maxwellian, with a deficit of periods in the range 8–10 hours.[24] The Maxwellian distribution of the rotational periods of Jupiter trojans may indicate that they have undergone a stronger collisional evolution compared to the asteroid belt.[24]

In 2008 a team from Calvin College examined the light curves of a debiased sample of ten Jupiter trojans, and found a median spin period of 18.9 hours. This value was significantly higher than that for main-belt asteroids of similar size (11.5 hours). The difference could mean that the Jupiter trojans possess a lower average density, which may imply that they formed in the Kuiper belt (see below).[25]

Composition

Spectroscopically, the Jupiter trojans mostly are D-type asteroids, which predominate in the outer regions of the asteroid belt.[5] A small number are classified as P or C-type asteroids.[24] Their spectra are red (meaning that they reflect more light at longer wavelengths) or neutral and featureless.[15] No firm evidence of water, organics or other chemical compounds has been obtained as of 2007. 4709 Ennomos has an albedo slightly higher than the Jupiter-trojan average, which may indicate the presence of water ice. Some other Jupiter Trojans, such as 911 Agamemnon and 617 Patroclus, have shown very weak absorptions at 1.7 and 2.3 μm, which might indicate the presence of organics.[26] The Jupiter trojans' spectra are similar to those of the irregular moons of Jupiter and, to a certain extent, comet nuclei, though Jupiter trojans are spectrally very different from the redder Kuiper belt objects.[1][5] A Jupiter trojan's spectrum can be matched to a mixture of water ice, a large amount of carbon-rich material (charcoal),[5] and possibly magnesium-rich silicates.[24] The composition of the Jupiter trojan population appears to be markedly uniform, with little or no differentiation between the two swarms.[27]

A team from the Keck Observatory in Hawaii announced in 2006 that it had measured the density of the binary Jupiter trojan 617 Patroclus as being less than that of water ice (0.8 g/cm3), suggesting that the pair, and possibly many other Trojan objects, more closely resemble comets or Kuiper belt objects in composition—water ice with a layer of dust—than they do the main-belt asteroids.[21] Countering this argument, the density of Hektor as determined from its rotational lightcurve (2.480 g/cm3) is significantly higher than that of 617 Patroclus.[23] Such a difference in densities suggests that density may not be a good indicator of asteroid origin.[23]

Origin and evolution

Two main theories have emerged to explain the formation and evolution of the Jupiter trojans. The first suggests that the Jupiter trojans formed in the same part of the Solar System as Jupiter and entered their orbits while it was forming.[10] The last stage of Jupiter's formation involved runaway growth of its mass through the accretion of large amounts of hydrogen and helium from the protoplanetary disk; during this growth, which lasted for only about 10,000 years, the mass of Jupiter increased by a factor of ten. The planetesimals that had approximately the same orbits as Jupiter were caught by the increased gravity of the planet.[10] The capture mechanism was very efficient—about 50% of all remaining planetesimals were trapped. This hypothesis has two major problems: the number of trapped bodies exceeds the observed population of Jupiter trojans by four orders of magnitude, and the present Jupiter trojan asteroids have larger orbital inclinations than are predicted by the capture model.[10] Simulations of this scenario show that such a mode of formation also would inhibit the creation of similar trojans for Saturn, and this has been borne out by observation: to date no trojans have been found near Saturn.[28] In a variation of this theory Jupiter captures trojans during its initial growth then migrates as it continues to grow. During Jupiter's migration the orbits of objects in horseshoe orbits are distorted causing the L4 side of these orbits to be over occupied. As a result, an excess of trojans is trapped on the L4 side when the horseshoe orbits shift to tadpole orbits as Jupiter grows. This model also leaves the Jupiter trojan population 3–4 orders of magnitude too large.[29]

The second theory proposes that the Jupiter trojans were captured during the migration of the giant planets described in the Nice model. In the Nice model the orbits of the giant planets became unstable 500–600 million years after the Solar System's formation when Jupiter and Saturn crossed their 1:2 mean-motion resonance. Encounters between planets resulted in Uranus and Neptune being scattered outward into the primordial Kuiper belt, disrupting it and throwing millions of objects inward.[30] When Jupiter and Saturn were near their 1:2 resonance the orbits of pre-existing Jupiter trojans became unstable during a secondary resonance with Jupiter and Saturn. This occurred when the period of the trojans' libration about their Lagrangian point had a 3:1 ratio to the period at which the position where Jupiter passes Saturn circulated relative to its perihelion. This process was also reversible allowing a fraction of the numerous objects scattered inward by Uranus and Neptune to enter this region and be captured as Jupiter's and Saturn's orbits separated. These new trojans had a wide range of inclinations, the result of multiple encounters with the giant planets before being captured.[31] This process can also occur later when Jupiter and Saturn cross weaker resonances.[32]

In a revised version of the Nice model Jupiter trojans are captured when Jupiter encounters an ice giant during the instability. In this version of the Nice model one of the ice giants (Uranus, Neptune, or a lost fifth planet) is scattered inward onto a Jupiter-crossing orbit and is scattered outward by Jupiter causing the orbits of Jupiter and Saturn to quickly separate. When Jupiter's semi-major axis jumps during these encounters existing Jupiter trojans can escape and new objects with semi-major axes similar to Jupiter's new semi-major axis are captured. Following its last encounter the ice giant can pass through one of the libration points and perturb their orbits leaving this libration point depleted relative to the other. After the encounters end some of these Jupiter trojans are lost and others captured when Jupiter and Saturn are near weak mean motion resonances such as the 3:7 resonance via the mechanism of the original Nice model.[32]

The long-term future of the Jupiter trojans is open to question, because multiple weak resonances with Jupiter and Saturn cause them to behave chaotically over time.[33] Collisional shattering slowly depletes the Jupiter trojan population as fragments are ejected. Ejected Jupiter trojans could become temporary satellites of Jupiter or Jupiter-family comets.[5] Simulations show that the orbits of up to 17% of Jupiter trojans are unstable over the age of the Solar System.[34] Levison et al. believe that roughly 200 ejected Jupiter trojans greater than 1 km in diameter might be travelling the Solar System, with a few possibly on Earth-crossing orbits.[35] Some of the escaped Jupiter trojans may become Jupiter-family comets as they approach the Sun and their surface ice begins evaporating.[35]

Exploration

On 4 January 2017 NASA announced that Lucy was selected as one of their next two Discovery Program missions.[36] Lucy is set to explore seven[37] Jupiter trojans. It launched on October 16, 2021, and will arrive at the L4 Trojan cloud in 2027 after two Earth gravity assists and a fly-by of a main-belt asteroid. It will then return to the vicinity of Earth for another gravity assist to take it to Jupiter's L5 Trojan cloud where it will visit 617 Patroclus.[38]

See also

Notes

  1. ^ The three other points—L1, L2 and L3—are unstable.[10]
  2. ^ The Maxwellian function is  , where   is the average rotational period,   is the dispersion of periods.

References

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External links

  • "Minor Planet Center's List of Trojan Minor Planets".
  • Sheppard, Scott. "The Trojan Page".
  • Lykawka, P. S.; Horner (2010). "The Capture of Trojan Asteroids by the Giant Planets During Planetary Migration". Monthly Notices of the Royal Astronomical Society. 405 (1383): 1375–1383. arXiv:1003.2137. Bibcode:2010MNRAS.405.1375L. doi:10.1111/j.1365-2966.2010.16538.x. S2CID 54084401.
  • NASA's WISE Colors in Unknowns on Jupiter Asteroids (NASA 2012-322 : 15 October 2012)
  • NASA's New Discovery Missions: Psyche and Lucy on YouTube
  • 3D Gravity Simulation of the Ten Largest Jupiter Trojan Asteroids 11 June 2020 at the Wayback Machine

jupiter, trojan, commonly, called, trojan, asteroids, simply, trojans, large, group, asteroids, that, share, planet, jupiter, orbit, around, relative, jupiter, each, trojan, librates, around, jupiter, stable, lagrange, points, either, existing, ahead, planet, . The Jupiter trojans commonly called trojan asteroids or simply trojans are a large group of asteroids that share the planet Jupiter s orbit around the Sun Relative to Jupiter each trojan librates around one of Jupiter s stable Lagrange points either L4 existing 60 ahead of the planet in its orbit or L5 60 behind Jupiter trojans are distributed in two elongated curved regions around these Lagrangian points with an average semi major axis of about 5 2 AU 1 The asteroids of the inner Solar System and Jupiter Jupiter trojans Hilda asteroids Asteroid belt Orbits of planets The Jupiter trojans are divided into two groups The Greek camp in front of and the Trojan camp trailing behind Jupiter in their orbit The first Jupiter trojan discovered 588 Achilles was spotted in 1906 by German astronomer Max Wolf 2 More than 9 800 Jupiter trojans have been found as of May 2021 update 3 By convention they are each named from Greek mythology after a figure of the Trojan War hence the name trojan The total number of Jupiter trojans larger than 1 km in diameter is believed to be about 1 million 1 approximately equal to the number of asteroids larger than 1 km in the asteroid belt 4 Like main belt asteroids Jupiter trojans form families 5 As of 2004 update many Jupiter trojans showed to observational instruments as dark bodies with reddish featureless spectra No firm evidence of the presence of water or any other specific compound on their surface has been obtained but it is thought that they are coated in tholins organic polymers formed by the Sun s radiation 6 The Jupiter trojans densities as measured by studying binaries or rotational lightcurves vary from 0 8 to 2 5 g cm 3 5 Jupiter trojans are thought to have been captured into their orbits during the early stages of the Solar System s formation or slightly later during the migration of giant planets 5 The term Trojan Asteroid specifically refers to the asteroids co orbital with Jupiter but the general term trojan is sometimes more generally applied to other small Solar System bodies with similar relationships to larger bodies Mars trojans Neptune trojans Uranus trojans and Earth trojans are known to exist 7 8 9 The term Trojan asteroid is normally understood to specifically mean the Jupiter trojans because the first Trojans were discovered near Jupiter s orbit and Jupiter currently has by far the most known Trojans 3 Contents 1 Observational history 2 Nomenclature 3 Numbers and mass 4 Orbits 4 1 Dynamical families and binaries 5 Physical properties 5 1 Rotation 5 2 Composition 6 Origin and evolution 7 Exploration 8 See also 9 Notes 10 References 11 External linksObservational history Edit Maximilian Franz Joseph Cornelius Wolf 1890 the discoverer of the first trojan In 1772 Italian born mathematician Joseph Louis Lagrange in studying the restricted three body problem predicted that a small body sharing an orbit with a planet but lying 60 ahead or behind it will be trapped near these points 2 The trapped body will librate slowly around the point of equilibrium in a tadpole or horseshoe orbit 10 These leading and trailing points are called the L4 and L5 Lagrange points 11 Note 1 The first asteroids trapped in Lagrange points were observed more than a century after Lagrange s hypothesis Those associated with Jupiter were the first to be discovered 2 E E Barnard made the first recorded observation of a trojan 12126 1999 RM11 identified as A904 RD at the time in 1904 but neither he nor others appreciated its significance at the time 12 Barnard believed he had seen the recently discovered Saturnian satellite Phoebe which was only two arc minutes away in the sky at the time or possibly an asteroid The object s identity was not understood until its orbit was calculated in 1999 12 The first accepted discovery of a trojan occurred in February 1906 when astronomer Max Wolf of Heidelberg Konigstuhl State Observatory discovered an asteroid at the L4 Lagrangian point of the Sun Jupiter system later named 588 Achilles 2 In 1906 1907 two more Jupiter trojans were found by fellow German astronomer August Kopff 624 Hektor and 617 Patroclus 2 Hektor like Achilles belonged to the L4 swarm ahead of the planet in its orbit whereas Patroclus was the first asteroid known to reside at the L5 Lagrangian point behind the planet 13 By 1938 11 Jupiter trojans had been detected 14 This number increased to 14 only in 1961 2 As instruments improved the rate of discovery grew rapidly by January 2000 a total of 257 had been discovered 11 by May 2003 the number had grown to 1 600 15 As of October 2018 update there are 4 601 known Jupiter trojans at L4 and 2 439 at L5 16 Nomenclature EditThe custom of naming all asteroids in Jupiter s L4 and L5 points after famous heroes of the Trojan War was suggested by Johann Palisa of Vienna who was the first to accurately calculate their orbits 2 Asteroids in the leading L4 orbit are named after Greek heroes the Greek node or camp or Achilles group and those at the trailing L5 orbit are named after the heroes of Troy the Trojan node or camp 2 The asteroids 617 Patroclus and 624 Hektor were named before the Greece Troy rule was devised resulting in a Greek spy Patroclus in the Trojan node and a Trojan spy Hector in the Greek node 14 17 Numbers and mass Edit A gravitational potential contour plot showing Earth s Lagrangian points L4 and L5 are ahead above and behind below the planet respectively Jupiter s Lagrangian points are similarly situated in its much larger orbit Estimates of the total number of Jupiter trojans are based on deep surveys of limited areas of the sky 1 The L4 swarm is believed to hold between 160 000 and 240 000 asteroids with diameters larger than 2 km and about 600 000 with diameters larger than 1 km 1 11 If the L5 swarm contains a comparable number of objects there are more than 1 million Jupiter trojans 1 km in size or larger For the objects brighter than absolute magnitude 9 0 the population is probably complete 15 These numbers are similar to that of comparable asteroids in the asteroid belt 1 The total mass of the Jupiter trojans is estimated at 0 0001 of the mass of Earth or one fifth of the mass of the asteroid belt 11 Two more recent studies indicate that the above numbers may overestimate the number of Jupiter trojans by several fold This overestimate is caused by 1 the assumption that all Jupiter trojans have a low albedo of about 0 04 whereas small bodies may have an average albedo as high as 0 12 18 2 an incorrect assumption about the distribution of Jupiter trojans in the sky 19 According to the new estimates the total number of Jupiter trojans with a diameter larger than 2 km is 6 300 1 000 and 3 400 500 in the L4 and L5 swarms respectively 19 These numbers would be reduced by a factor of 2 if small Jupiter trojans are more reflective than large ones 18 The number of Jupiter trojans observed in the L4 swarm is slightly larger than that observed in L5 Because the brightest Jupiter trojans show little variation in numbers between the two populations this disparity is probably due to observational bias 5 Some models indicate that the L4 swarm may be slightly more stable than the L5 swarm 10 The largest Jupiter trojan is 624 Hektor which has a mean diameter of 203 3 6 km 15 There are few large Jupiter trojans in comparison to the overall population With decreasing size the number of Jupiter trojans grows very quickly down to 84 km much more so than in the asteroid belt A diameter of 84 km corresponds to an absolute magnitude of 9 5 assuming an albedo of 0 04 Within the 4 4 40 km range the Jupiter trojans size distribution resembles that of the main belt asteroids Nothing is known about the masses of the smaller Jupiter trojans 10 The size distribution suggests that the smaller Trojans may be the products of collisions by larger Jupiter trojans 5 The largest Jupiter trojans Trojan Diameter km 624 Hektor 225617 Patroclus 140911 Agamemnon 131588 Achilles 1303451 Mentor 1263317 Paris 1191867 Deiphobus 1181172 Aneas 1181437 Diomedes 1181143 Odysseus 115Source JPL Small Body Database NEOWISE dataOrbits Edit Animation of the orbit of 624 Hektor blue set against the orbit of Jupiter outer red ellipse Jupiter trojans have orbits with radii between 5 05 and 5 35 AU the mean semi major axis is 5 2 0 15 AU and are distributed throughout elongated curved regions around the two Lagrangian points 1 each swarm stretches for about 26 along the orbit of Jupiter amounting to a total distance of about 2 5 AU 11 The width of the swarms approximately equals two Hill s radii which in the case of Jupiter amounts to about 0 6 AU 10 Many of Jupiter trojans have large orbital inclinations relative to Jupiter s orbital plane up to 40 11 Jupiter trojans do not maintain a fixed separation from Jupiter They slowly librate around their respective equilibrium points periodically moving closer to Jupiter or farther from it 10 Jupiter trojans generally follow paths called tadpole orbits around the Lagrangian points the average period of their libration is about 150 years 11 The amplitude of the libration along the Jovian orbit varies from 0 6 to 88 with the average being about 33 10 Simulations show that Jupiter trojans can follow even more complicated trajectories when moving from one Lagrangian point to another these are called horseshoe orbits currently no Jupiter Trojan with such an orbit is known though one is known for Neptune 10 Dynamical families and binaries Edit Discerning dynamical families within the Jupiter trojan population is more difficult than it is in the asteroid belt because the Jupiter trojans are locked within a far narrower range of possible positions This means that clusters tend to overlap and merge with the overall swarm By 2003 roughly a dozen dynamical families were identified Jupiter trojan families are much smaller in size than families in the asteroid belt the largest identified family the Menelaus group consists of only eight members 5 In 2001 617 Patroclus was the first Jupiter trojan to be identified as a binary asteroid 20 The binary s orbit is extremely close at 650 km compared to 35 000 km for the primary s Hill sphere 21 The largest Jupiter trojan 624 Hektor is probably a contact binary with a moonlet 5 22 23 Physical properties Edit Trojan 624 Hektor indicated is similar in brightness to dwarf planet Pluto Jupiter trojans are dark bodies of irregular shape Their geometric albedos generally vary between 3 and 10 15 The average value is 0 056 0 003 for the objects larger than 57 km 5 and 0 121 0 003 R band for those smaller than 25 km 18 The asteroid 4709 Ennomos has the highest albedo 0 18 of all known Jupiter trojans 15 Little is known about the masses chemical composition rotation or other physical properties of the Jupiter trojans 5 Rotation Edit The rotational properties of Jupiter trojans are not well known Analysis of the rotational light curves of 72 Jupiter trojans gave an average rotational period of about 11 2 hours whereas the average period of the control sample of asteroids in the asteroid belt was 10 6 hours 24 The distribution of the rotational periods of Jupiter trojans appeared to be well approximated by a Maxwellian function Note 2 whereas the distribution for main belt asteroids was found to be non Maxwellian with a deficit of periods in the range 8 10 hours 24 The Maxwellian distribution of the rotational periods of Jupiter trojans may indicate that they have undergone a stronger collisional evolution compared to the asteroid belt 24 In 2008 a team from Calvin College examined the light curves of a debiased sample of ten Jupiter trojans and found a median spin period of 18 9 hours This value was significantly higher than that for main belt asteroids of similar size 11 5 hours The difference could mean that the Jupiter trojans possess a lower average density which may imply that they formed in the Kuiper belt see below 25 Composition Edit Spectroscopically the Jupiter trojans mostly are D type asteroids which predominate in the outer regions of the asteroid belt 5 A small number are classified as P or C type asteroids 24 Their spectra are red meaning that they reflect more light at longer wavelengths or neutral and featureless 15 No firm evidence of water organics or other chemical compounds has been obtained as of 2007 update 4709 Ennomos has an albedo slightly higher than the Jupiter trojan average which may indicate the presence of water ice Some other Jupiter Trojans such as 911 Agamemnon and 617 Patroclus have shown very weak absorptions at 1 7 and 2 3 mm which might indicate the presence of organics 26 The Jupiter trojans spectra are similar to those of the irregular moons of Jupiter and to a certain extent comet nuclei though Jupiter trojans are spectrally very different from the redder Kuiper belt objects 1 5 A Jupiter trojan s spectrum can be matched to a mixture of water ice a large amount of carbon rich material charcoal 5 and possibly magnesium rich silicates 24 The composition of the Jupiter trojan population appears to be markedly uniform with little or no differentiation between the two swarms 27 A team from the Keck Observatory in Hawaii announced in 2006 that it had measured the density of the binary Jupiter trojan 617 Patroclus as being less than that of water ice 0 8 g cm3 suggesting that the pair and possibly many other Trojan objects more closely resemble comets or Kuiper belt objects in composition water ice with a layer of dust than they do the main belt asteroids 21 Countering this argument the density of Hektor as determined from its rotational lightcurve 2 480 g cm3 is significantly higher than that of 617 Patroclus 23 Such a difference in densities suggests that density may not be a good indicator of asteroid origin 23 Origin and evolution EditTwo main theories have emerged to explain the formation and evolution of the Jupiter trojans The first suggests that the Jupiter trojans formed in the same part of the Solar System as Jupiter and entered their orbits while it was forming 10 The last stage of Jupiter s formation involved runaway growth of its mass through the accretion of large amounts of hydrogen and helium from the protoplanetary disk during this growth which lasted for only about 10 000 years the mass of Jupiter increased by a factor of ten The planetesimals that had approximately the same orbits as Jupiter were caught by the increased gravity of the planet 10 The capture mechanism was very efficient about 50 of all remaining planetesimals were trapped This hypothesis has two major problems the number of trapped bodies exceeds the observed population of Jupiter trojans by four orders of magnitude and the present Jupiter trojan asteroids have larger orbital inclinations than are predicted by the capture model 10 Simulations of this scenario show that such a mode of formation also would inhibit the creation of similar trojans for Saturn and this has been borne out by observation to date no trojans have been found near Saturn 28 In a variation of this theory Jupiter captures trojans during its initial growth then migrates as it continues to grow During Jupiter s migration the orbits of objects in horseshoe orbits are distorted causing the L4 side of these orbits to be over occupied As a result an excess of trojans is trapped on the L4 side when the horseshoe orbits shift to tadpole orbits as Jupiter grows This model also leaves the Jupiter trojan population 3 4 orders of magnitude too large 29 The second theory proposes that the Jupiter trojans were captured during the migration of the giant planets described in the Nice model In the Nice model the orbits of the giant planets became unstable 500 600 million years after the Solar System s formation when Jupiter and Saturn crossed their 1 2 mean motion resonance Encounters between planets resulted in Uranus and Neptune being scattered outward into the primordial Kuiper belt disrupting it and throwing millions of objects inward 30 When Jupiter and Saturn were near their 1 2 resonance the orbits of pre existing Jupiter trojans became unstable during a secondary resonance with Jupiter and Saturn This occurred when the period of the trojans libration about their Lagrangian point had a 3 1 ratio to the period at which the position where Jupiter passes Saturn circulated relative to its perihelion This process was also reversible allowing a fraction of the numerous objects scattered inward by Uranus and Neptune to enter this region and be captured as Jupiter s and Saturn s orbits separated These new trojans had a wide range of inclinations the result of multiple encounters with the giant planets before being captured 31 This process can also occur later when Jupiter and Saturn cross weaker resonances 32 In a revised version of the Nice model Jupiter trojans are captured when Jupiter encounters an ice giant during the instability In this version of the Nice model one of the ice giants Uranus Neptune or a lost fifth planet is scattered inward onto a Jupiter crossing orbit and is scattered outward by Jupiter causing the orbits of Jupiter and Saturn to quickly separate When Jupiter s semi major axis jumps during these encounters existing Jupiter trojans can escape and new objects with semi major axes similar to Jupiter s new semi major axis are captured Following its last encounter the ice giant can pass through one of the libration points and perturb their orbits leaving this libration point depleted relative to the other After the encounters end some of these Jupiter trojans are lost and others captured when Jupiter and Saturn are near weak mean motion resonances such as the 3 7 resonance via the mechanism of the original Nice model 32 The long term future of the Jupiter trojans is open to question because multiple weak resonances with Jupiter and Saturn cause them to behave chaotically over time 33 Collisional shattering slowly depletes the Jupiter trojan population as fragments are ejected Ejected Jupiter trojans could become temporary satellites of Jupiter or Jupiter family comets 5 Simulations show that the orbits of up to 17 of Jupiter trojans are unstable over the age of the Solar System 34 Levison et al believe that roughly 200 ejected Jupiter trojans greater than 1 km in diameter might be travelling the Solar System with a few possibly on Earth crossing orbits 35 Some of the escaped Jupiter trojans may become Jupiter family comets as they approach the Sun and their surface ice begins evaporating 35 Exploration EditOn 4 January 2017 NASA announced that Lucy was selected as one of their next two Discovery Program missions 36 Lucy is set to explore seven 37 Jupiter trojans It launched on October 16 2021 and will arrive at the L4 Trojan cloud in 2027 after two Earth gravity assists and a fly by of a main belt asteroid It will then return to the vicinity of Earth for another gravity assist to take it to Jupiter s L5 Trojan cloud where it will visit 617 Patroclus 38 See also EditComet Shoemaker Levy 9 List of Jupiter trojans Greek camp List of Jupiter trojans Trojan camp List of Jupiter crossing minor planets List of objects at Lagrangian pointsNotes Edit The three other points L1 L2 and L3 are unstable 10 The Maxwellian function is F 1 2 p s P 2 exp P P 0 2 s 2 displaystyle F begin smallmatrix frac 1 sqrt 2 pi sigma P 2 exp P P 0 2 sigma 2 end smallmatrix where P 0 displaystyle P 0 is the average rotational period s displaystyle sigma is the dispersion of periods References Edit a b c d e f g Yoshida F Nakamura T 2005 Size distribution of faint L4 Trojan asteroids The Astronomical Journal 130 6 2900 11 Bibcode 2005AJ 130 2900Y doi 10 1086 497571 a b c d e f g h Nicholson Seth B 1961 The Trojan asteroids Astronomical Society of the Pacific Leaflets 8 381 239 46 Bibcode 1961ASPL 8 239N a b Trojan Minor Planets Minor Planet Center Archived from the original on 29 June 2017 Retrieved 14 October 2018 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1393 1408 arXiv astro ph 0612237 Bibcode 2007AJ 133 1393L doi 10 1086 511772 S2CID 17735600 a b c d e Barucci M A Kruikshank D P Mottola S Lazzarin M 2002 Physical Properties of Trojan and Centaur Asteroids Asteroids III Tucson Arizona University of Arizona Press pp 273 87 Molnar Lawrence A Haegert Melissa J Hoogeboom Kathleen M April 2008 Lightcurve Analysis of an Unbiased Sample of Trojan Asteroids The Minor Planet Bulletin Association of Lunar and Planetary Observers 35 2 82 84 Bibcode 2008MPBu 35 82M OCLC 85447686 Yang Bin Jewitt David 2007 Spectroscopic Search for Water Ice on Jovian Trojan Asteroids The Astronomical Journal 134 1 223 228 Bibcode 2007AJ 134 223Y doi 10 1086 518368 Retrieved 19 January 2009 Dotto E Fornasier S Barucci M A et al August 2006 The surface composition of Jupiter trojans Visible and near infrared survey of dynamical families Icarus 183 2 420 434 Bibcode 2006Icar 183 420D doi 10 1016 j icarus 2006 02 012 Marzari F Scholl H 1998 The growth of Jupiter and Saturn and the capture of Trojans Astronomy and Astrophysics 339 278 285 Bibcode 1998A amp A 339 278M Pirani S Johansen A Bitsch B Mustill A J Turrini D 2019 Consequences of planetary migration on the minor bodies of the early solar system Astronomy amp Astrophysics 623 A169 arXiv 1902 04591 Bibcode 2019A amp A 623A 169P doi 10 1051 0004 6361 201833713 S2CID 119546182 Levison Harold F Morbidelli Alessandro Van Laerhoven Christa et al 2007 Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune Icarus 196 1 258 273 arXiv 0712 0553 Bibcode 2008Icar 196 258L doi 10 1016 j icarus 2007 11 035 S2CID 7035885 Morbidelli A Levison H F Tsiganis K Gomes R 26 May 2005 Chaotic capture of Jupiter s Trojan asteroids in the early Solar System PDF Nature 435 7041 462 465 Bibcode 2005Natur 435 462M doi 10 1038 nature03540 OCLC 112222497 PMID 15917801 S2CID 4373366 Archived from the original PDF on 31 July 2009 Retrieved 19 January 2009 a b Nesvorny David Vokrouhlicky David Morbidelli Alessandro 2013 Capture of Trojans by Jumping Jupiter The Astrophysical Journal 768 1 45 arXiv 1303 2900 Bibcode 2013ApJ 768 45N doi 10 1088 0004 637X 768 1 45 S2CID 54198242 Robutal P Gabern F Jorba A 2005 The observed Trojans and the global dynamics around the lagrangian points of the sun jupiter system PDF Celestial Mechanics and Dynamical Astronomy 92 1 3 53 69 Bibcode 2005CeMDA 92 53R doi 10 1007 s10569 004 5976 y S2CID 5759776 Archived from the original PDF on 31 July 2009 Kleomenis Tsiganis Harry Varvoglis Rudolf Dvorak April 2005 Chaotic Diffusion And Effective Stability of Jupiter trojans Celestial Mechanics and Dynamical Astronomy Springer 92 1 3 71 87 Bibcode 2005CeMDA 92 71T doi 10 1007 s10569 004 3975 7 S2CID 123648472 a b Levison Harold F Shoemaker Eugene M Shoemaker Carolyn S 1997 Dynamical evolution of Jupiter s Trojan asteroids Nature 385 6611 42 44 Bibcode 1997Natur 385 42L doi 10 1038 385042a0 S2CID 4323757 Northon Karen 4 January 2017 NASA Selects Two Missions to Explore the Early Solar System NASA Archived from the original on 5 January 2017 Retrieved 5 January 2017 Tour Lucy Mission Website NASA Retrieved 5 October 2021 Dreier Casey Lakdawalla Emily 30 September 2015 NASA announces five Discovery proposals selected for further study The Planetary Society Archived from the original on 2 October 2015 Retrieved 1 October 2015 External links Edit Wikimedia Commons has media related to Jupiter trojans Minor Planet Center s List of Trojan Minor Planets Sheppard Scott The Trojan Page Lykawka P S Horner 2010 The Capture of Trojan Asteroids by the Giant Planets During Planetary Migration Monthly Notices of the Royal Astronomical Society 405 1383 1375 1383 arXiv 1003 2137 Bibcode 2010MNRAS 405 1375L doi 10 1111 j 1365 2966 2010 16538 x S2CID 54084401 NASA s WISE Colors in Unknowns on Jupiter Asteroids NASA 2012 322 15 October 2012 NASA s New Discovery Missions Psyche and Lucy on YouTube 3D Gravity Simulation of the Ten Largest Jupiter Trojan Asteroids Archived 11 June 2020 at the Wayback Machine Portals Astronomy Stars Spaceflight Outer space Solar system Retrieved from https en wikipedia org w index php title Jupiter trojan amp oldid 1141920589, wikipedia, wiki, book, books, library,

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