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Scattered disc

From Wikipedia, the free encyclopedia

Eris, the largest known scattered-disc object (center), and its moon Dysnomia (left of object)
Eris, the largest known scattered-disc object (center), and its moon Dysnomia (left of object)

The scattered disc (or scattered disk) is a distant circumstellar disc in the Solar System that is sparsely populated by icy small solar system bodies, which are a subset of the broader family of trans-Neptunian objects. The scattered-disc objects (SDOs) have orbital eccentricities ranging as high as 0.8, inclinations as high as 40°, and perihelia greater than 30 astronomical units (4.5×109 km; 2.8×109 mi). These extreme orbits are thought to be the result of gravitational "scattering" by the gas giants, and the objects continue to be subject to perturbation by the planet Neptune.

Although the closest scattered-disc objects approach the Sun at about 30–35 AU, their orbits can extend well beyond 100 AU. This makes scattered objects among the coldest and most distant objects in the Solar System.[1] The innermost portion of the scattered disc overlaps with a torus-shaped region of orbiting objects traditionally called the Kuiper belt,[2] but its outer limits reach much farther away from the Sun and farther above and below the ecliptic than the Kuiper belt proper.[a]

Because of its unstable nature, astronomers now consider the scattered disc to be the place of origin for most periodic comets in the Solar System, with the centaurs, a population of icy bodies between Jupiter and Neptune, being the intermediate stage in an object's migration from the disc to the inner Solar System.[4] Eventually, perturbations from the giant planets send such objects towards the Sun, transforming them into periodic comets. Many objects of the proposed Oort cloud are also thought to have originated in the scattered disc. Detached objects are not sharply distinct from scattered disc objects, and some such as Sedna have sometimes been considered to be included in this group.

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  • ✪ Life Beyond Neptune: The Kuiper Belt & Scattered Disc
  • ✪ The Oort Cloud: Crash Course Astronomy #22
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  • ✪ Where Is The Edge Of The Solar System?
  • ✪ Pluto - Visitors from the Kuiper Belt


[♪ INTRO] It might not always seem like much, but the solar system is a really big place. It’s almost stupidly big. Normally, we just think about the planets and maybe the asteroid belt, but it includes a lot more than that. And to make sense of it all, astronomers break things up into regions where the objects are more or less similar. Beyond Neptune, and before you get to a group of icy objects called the Oort Cloud, there are two big transition regions called the Kuiper Belt and the scattered disc, and together, they form the frontier of modern planetary science. The Kuiper Belt stretches from about 30 to 55 astronomical units, or AU. One AU is the average distance from the Earth to the Sun, and astronomers use it to describe large distances. After about 55 AU, the scattered disc starts. The objects in both these regions are the frozen leftovers of when the planets formed. Back in the early history of the solar system, they were all tossed around when the giant planets migrated outward. Kind of like when you go grocery shopping and push your leftovers to the back of the fridge. Now, the Kuiper Belt is mostly known for being full of icy objects, like comets, or for being home to Pluto. But it’s actually defined by something a heck of a lot bigger: Neptune. Neptune basically rules the Kuiper Belt. It influences the orbits of most objects that exist there because of an effect called a mean motion resonance. These resonances happen at spots where Kuiper Belt objects orbit the Sun in a nice, even ratio with Neptune. For example, Pluto’s trapped in a 2:3 resonance, meaning it orbits the Sun exactly twice for every three orbits Neptune makes. And that keeps Pluto from flying off course. Not all Kuiper Belt objects are in resonance with Neptune, but they’re still close enough to be affected by it in some way. And in the region as a whole, these resonances are a stabilizing force and define what it means to be in the Kuiper Belt. Beyond about 55 AU, Neptune’s influence become weaker and less important. That’s where the scattered disc starts, and it extends all the way to the edge of the Oort Cloud, thousands of AU from the Sun. Objects in the scattered disc are… well, scattered. For once, astronomers actually gave something a useful name. Instead of being neatly ordered by Neptune’s gravity, these objects are much more likely to be disrupted by it, and that can throw them into some extreme orbits. Take Eris, a dwarf planet in the scattered disc. Its orbit carries it anywhere from 38 to 98 AU, and it’s also tilted by 45 degrees, which means it usually is way above or below the plane of the solar system. Now, even though we use physics to draw distinctions between the Kuiper Belt and the scattered disc, the worlds in both regions are probably pretty similar. They’re mostly big balls of ice, but that is definitely not as boring as it sounds. These regions are normally way more exciting and interesting than anything we could’ve imagined. In 2015, when New Horizons flew by Pluto and its moon Charon, it was our first real experience with the Kuiper Belt, and it showed us a ton of weird stuff. For one, their surfaces are covered in a strange organic substance astronomers call tholins, and they even seem to exchange the ingredients to make tholins back and forth. Also, two of Pluto’s smaller moons, Nix and Hydra, both rotate chaotically, which means it’s literally impossible to predict how they’ll spin in the future. Then, outside the Pluto system, there’s Haumea, another object in the Kuiper Belt slightly smaller than Pluto. This year, scientists discovered that Haumea has a ring, making it the farthest known ring system in the entire solar system! Basically, the Kuiper Belt is packed with variety, and we’re still figuring out what other objects might exist there. And since many objects in the scattered disc have extremely elongated orbits, they might be totally new kinds of strange. Even in the Kuiper Belt, changing temperatures over Pluto’s elliptical orbit means that its atmosphere can more than triple in pressure over the course of a Pluto year, which is pretty dang weird. Imagine being on Earth and getting squished by the atmosphere every few months. So who knows what’s hiding in the scattered disc. To find out the true range of possibilities, we’ll need to study some more objects. Unfortunately, the scattered disc is hard to research because it’s really dark that far from the Sun, and it’s hard to get clear images with our telescopes. And sending a probe there would take decades. So for now, we’ll focus on learning more about the Kuiper Belt. And New Horizons is gonna make that happen. On New Year’s Day 2019, it’ll fly by a Kuiper Belt object called 2014 MU69. It might be what scientists call a contact binary, a pair of objects that orbit each other so closely that they might even touch! But we’ll know more soon. Sadly, after New Horizons is finished, the Kuiper Belt and scattered disc will go back to just being points of light to us. But we’ve already learned a ton about them, and now we’ve got a whole new appreciation for all those weird worlds out there. Thanks for watching this episode of SciShow Space! If you’d like to learn more about what comes after the scattered disc, you can check out another one of our episodes, where I tell you all about the Oort Cloud! [♪ OUTRO]



Traditionally, devices like a blink comparator were used in astronomy to detect objects in the Solar System, because these objects would move between two exposures—this involved time-consuming steps like exposing and developing photographic plates or films, and people then using a blink comparator to manually detect prospective objects. During the 1980s, the use of CCD-based cameras in telescopes made it possible to directly produce electronic images that could then be readily digitized and transferred to digital images. Because the CCD captured more light than film (about 90% versus 10% of incoming light) and the blinking could now be done at an adjustable computer screen, the surveys allowed for higher throughput. A flood of new discoveries was the result: over a thousand trans-Neptunian objects were detected between 1992 and 2006.[5]

The first scattered-disc object (SDO) to be recognised as such was 1996 TL66,[6][7] originally identified in 1996 by astronomers based at Mauna Kea in Hawaii. Three more were identified by the same survey in 1999: 1999 CV<sub>118</sub>, 1999 CY118, and 1999 CF119.[8] The first object presently classified as an SDO to be discovered was 1995 TL8, found in 1995 by Spacewatch.[9]

As of 2011, over 200 SDOs have been identified,[10] including Gǃkúnǁʼhòmdímà (discovered by Schwamb, Brown, and Rabinowitz),[11] 2002 TC302 (NEAT), Eris (Brown, Trujillo, and Rabinowitz),[12] Sedna (Brown, Trujillo, and Rabinowitz)[13] and 2004 VN112 (Deep Ecliptic Survey).[14] Although the numbers of objects in the Kuiper belt and the scattered disc are hypothesized to be roughly equal, observational bias due to their greater distance means that far fewer SDOs have been observed to date.[15]

Subdivisions of trans-Neptunian space

The eccentricity and inclination of the scattered-disc population compared to the classical and 5:2 resonant Kuiper-belt objects
The eccentricity and inclination of the scattered-disc population compared to the classical and 5:2 resonant Kuiper-belt objects

Known trans-Neptunian objects are often divided into two subpopulations: the Kuiper belt and the scattered disc.[16] A third reservoir of trans-Neptunian objects, the Oort cloud, has been hypothesized, although no confirmed direct observations of the Oort cloud have been made.[2] Some researchers further suggest a transitional space between the scattered disc and the inner Oort cloud, populated with "detached objects".[17]

Scattered disc versus Kuiper belt

The Kuiper belt is a relatively thick torus (or "doughnut") of space, extending from about 30 to 50 AU[18] comprising two main populations of Kuiper belt objects (KBOs): the classical Kuiper-belt objects (or "cubewanos"), which lie in orbits untouched by Neptune, and the resonant Kuiper-belt objects; those which Neptune has locked into a precise orbital ratio such as 2:3 (the object goes around twice for every three Neptune orbits) and 1:2 (the object goes around once for every two Neptune orbits). These ratios, called orbital resonances, allow KBOs to persist in regions which Neptune's gravitational influence would otherwise have cleared out over the age of the Solar System, since the objects are never close enough to Neptune to be scattered by its gravity. Those in 2:3 resonances are known as "plutinos", because Pluto is the largest member of their group, whereas those in 1:2 resonances are known as "twotinos".

In contrast to the Kuiper belt, the scattered-disc population can be disturbed by Neptune.[19] Scattered-disc objects come within gravitational range of Neptune at their closest approaches (~30 AU) but their farthest distances reach many times that.[17] Ongoing research[20] suggests that the centaurs, a class of icy planetoids that orbit between Jupiter and Neptune, may simply be SDOs thrown into the inner reaches of the Solar System by Neptune, making them "cis-Neptunian" rather than trans-Neptunian scattered objects.[21] Some objects, like (29981) 1999 TD10, blur the distinction[22] and the Minor Planet Center (MPC), which officially catalogues all trans-Neptunian objects, now lists centaurs and SDOs together.[10]

The MPC, however, makes a clear distinction between the Kuiper belt and the scattered disc, separating those objects in stable orbits (the Kuiper belt) from those in scattered orbits (the scattered disc and the centaurs).[10] However, the difference between the Kuiper belt and the scattered disc is not clear-cut, and many astronomers see the scattered disc not as a separate population but as an outward region of the Kuiper belt. Another term used is "scattered Kuiper-belt object" (or SKBO) for bodies of the scattered disc.[23]

Morbidelli and Brown propose that the difference between objects in the Kuiper belt and scattered-disc objects is that the latter bodies "are transported in semi-major axis by close and distant encounters with Neptune,"[16] but the former experienced no such close encounters. This delineation is inadequate (as they note) over the age of the Solar System, since bodies "trapped in resonances" could "pass from a scattering phase to a non-scattering phase (and vice versa) numerous times."[16] That is, trans-Neptunian objects could travel back and forth between the Kuiper belt and the scattered disc over time. Therefore, they chose instead to define the regions, rather than the objects, defining the scattered disc as "the region of orbital space that can be visited by bodies that have encountered Neptune" within the radius of a Hill sphere, and the Kuiper belt as its "complement ... in the a > 30 AU region"; the region of the Solar System populated by objects with semi-major axes greater than 30 AU.[16]

Detached objects

The Minor Planet Center classifies the trans-Neptunian object 90377 Sedna as a scattered-disc object. Its discoverer Michael E. Brown has suggested instead that it should be considered an inner Oort-cloud object rather than a member of the scattered disc, because, with a perihelion distance of 76 AU, it is too remote to be affected by the gravitational attraction of the outer planets. [24] Under this definition, an object with a perihelion greater than 40 AU could be classified as outside the scattered disc. [25]

Sedna is not the only such object: (148209) 2000 CR105 (discovered before Sedna) and 2004 VN112 have a perihelion too far away from Neptune to be influenced by it. This led to a discussion among astronomers about a new minor planet set, called the extended scattered disc (E-SDO). [26] 2000 CR105 may also be an inner Oort-cloud object or (more likely) a transitional object between the scattered disc and the inner Oort cloud. More recently, these objects have been referred to as "detached",[27] or distant detached objects (DDO).[28]

There are no clear boundaries between the scattered and detached regions.[25] Gomes et al. define SDOs as having "highly eccentric orbits, perihelia beyond Neptune, and semi-major axes beyond the 1:2 resonance." By this definition, all distant detached objects are SDOs.[17] Since detached objects' orbits cannot be produced by Neptune scattering, alternative scattering mechanisms have been put forward, including a passing star[29] or a distant, planet-sized object.[28]

A scheme introduced by a 2005 report from the Deep Ecliptic Survey by J. L. Elliott et al. distinguishes between two categories: scattered-near (i.e. typical SDOs) and scattered-extended (i.e. detached objects).[30] Scattered-near objects are those whose orbits are non-resonant, non-planetary-orbit-crossing and have a Tisserand parameter (relative to Neptune) less than 3.[30] Scattered-extended objects have a Tisserand parameter (relative to Neptune) greater than 3 and have a time-averaged eccentricity greater than 0.2.[30]

An alternative classification, introduced by B. J. Gladman, B. G. Marsden and C. Van Laerhoven in 2007, uses 10-million-year orbit integration instead of the Tisserand parameter.[31] An object qualifies as an SDO if its orbit is not resonant, has a semi-major axis no greater than 2000 AU, and, during the integration, its semi-major axis shows an excursion of 1.5 AU or more.[31] Gladman et al. suggest the term scattering disk object to emphasize this present mobility.[31] If the object is not an SDO as per the above definition, but the eccentricity of its orbit is greater than 0.240, it is classified as a detached TNO.[31] (Objects with smaller eccentricity are considered classical.) In this scheme, the disc extends from the orbit of Neptune to 2000 AU, the region referred to as the inner Oort cloud.


Distribution of trans-Neptunian objects, with semi-major axis on the horizontal, and inclination on the vertical axis. Scattered disc objects are shown in grey, objects that are in resonance with Neptune in red. Classical Kuiper belt objects (cubewanos) and sednoids are blue and yellow, respectively.
Distribution of trans-Neptunian objects, with semi-major axis on the horizontal, and inclination on the vertical axis. Scattered disc objects are shown in grey, objects that are in resonance with Neptune in red. Classical Kuiper belt objects (cubewanos) and sednoids are blue and yellow, respectively.

The scattered disc is a very dynamic environment.[15] Because they are still capable of being perturbed by Neptune, SDOs' orbits are always in danger of disruption; either of being sent outward to the Oort cloud or inward into the centaur population and ultimately the Jupiter family of comets.[15] For this reason Gladman et al. prefer to refer to the region as the scattering disc, rather than scattered.[31] Unlike Kuiper-belt objects (KBOs), the orbits of scattered-disc objects can be inclined as much as 40° from the ecliptic.[32]

SDOs are typically characterized by orbits with medium and high eccentricities with a semi-major axis greater than 50 AU, but their perihelia bring them within influence of Neptune.[33] Having a perihelion of roughly 30 AU is one of the defining characteristics of scattered objects, as it allows Neptune to exert its gravitational influence.[8]

The classical objects (cubewanos) are very different from the scattered objects: more than 30% of all cubewanos are on low-inclination, near-circular orbits whose eccentricities peak at 0.25.[34] Classical objects possess eccentricities ranging from 0.2 to 0.8. Though the inclinations of scattered objects are similar to the more extreme KBOs, very few scattered objects have orbits as close to the ecliptic as much of the KBO population.[15]

Although motions in the scattered disc are random, they do tend to follow similar directions, which means that SDOs can become trapped in temporary resonances with Neptune. Examples of possible resonant orbits within the scattered disc include 1:3, 2:7, 3:11, 5:22 and 4:79.[17]


Simulation showing Outer Planets and Kuiper Belt: a) Before Jupiter/Saturn 2:1 resonance b) Scattering of Kuiper-belt objects into the Solar System after the orbital shift of Neptune c) After ejection of Kuiper-belt bodies by Jupiter
Simulation showing Outer Planets and Kuiper Belt: a) Before Jupiter/Saturn 2:1 resonance b) Scattering of Kuiper-belt objects into the Solar System after the orbital shift of Neptune c) After ejection of Kuiper-belt bodies by Jupiter

The scattered disc is still poorly understood: no model of the formation of the Kuiper belt and the scattered disc has yet been proposed that explains all their observed properties.[16]

According to contemporary models, the scattered disc formed when Kuiper belt objects (KBOs) were "scattered" into eccentric and inclined orbits by gravitational interaction with Neptune and the other outer planets.[35] The amount of time for this process to occur remains uncertain. One hypothesis estimates a period equal to the entire age of the Solar System;[36] a second posits that the scattering took place relatively quickly, during Neptune's early migration epoch.[37]

Models for a continuous formation throughout the age of the Solar System illustrate that at weak resonances within the Kuiper belt (such as 5:7 or 8:1), or at the boundaries of stronger resonances, objects can develop weak orbital instabilities over millions of years. The 4:7 resonance in particular has large instability. KBOs can also be shifted into unstable orbits by close passage of massive objects, or through collisions. Over time, the scattered disc would gradually form from these isolated events.[17]

Computer simulations have also suggested a more rapid and earlier formation for the scattered disc. Modern theories indicate that neither Uranus nor Neptune could have formed in situ beyond Saturn, as too little primordial matter existed at that range to produce objects of such high mass. Instead, these planets, and Saturn, may have formed closer to Jupiter, but were flung outwards during the early evolution of the Solar System, perhaps through exchanges of angular momentum with scattered objects.[38] Once the orbits of Jupiter and Saturn shifted to a 2:1 resonance (two Jupiter orbits for each orbit of Saturn), their combined gravitational pull disrupted the orbits of Uranus and Neptune, sending Neptune into the temporary "chaos" of the proto-Kuiper belt.[37] As Neptune traveled outward, it scattered many trans-Neptunian objects into higher and more eccentric orbits.[35][39] This model states that 90% or more of the objects in the scattered disc may have been "promoted into these eccentric orbits by Neptune's resonances during the migration epoch...[therefore] the scattered disc might not be so scattered."[38]


The infrared spectra of both Eris and Pluto, highlighting their common methane absorption lines
The infrared spectra of both Eris and Pluto, highlighting their common methane absorption lines

Scattered objects, like other trans-Neptunian objects, have low densities and are composed largely of frozen volatiles such as water and methane.[40] Spectral analysis of selected Kuiper belt and scattered objects has revealed signatures of similar compounds. Both Pluto and Eris, for instance, show signatures for methane.[41]

Astronomers originally supposed that the entire trans-Neptunian population would show a similar red surface colour, as they were thought to have originated in the same region and subjected to the same physical processes.[40] Specifically, SDOs were expected to have large amounts of surface methane, chemically altered into complex organic molecules by energy from the Sun. This would absorb blue light, creating a reddish hue.[40] Most classical objects display this colour, but scattered objects do not; instead, they present a white or greyish appearance.[40]

One explanation is the exposure of whiter subsurface layers by impacts; another is that the scattered objects' greater distance from the Sun creates a composition gradient, analogous to the composition gradient of the terrestrial and gas giant planets.[40] Michael E. Brown, discoverer of the scattered object Eris, suggests that its paler colour could be because, at its current distance from the Sun, its atmosphere of methane is frozen over its entire surface, creating an inches-thick layer of bright white ice. Pluto, conversely, being closer to the Sun, would be warm enough that methane would freeze only onto cooler, high-albedo regions, leaving low-albedo tholin-covered regions bare of ice.[41]


The Kuiper belt was initially thought to be the source of the Solar System's ecliptic comets. However, studies of the region since 1992 have shown that the orbits within the Kuiper belt are relatively stable, and that ecliptic comets originate from the scattered disc, where orbits are generally less stable.[42]

Comets can loosely be divided into two categories: short-period and long-period—the latter being thought to originate in the Oort cloud. The two major categories of short-period comets are Jupiter-family comets (JFCs) and Halley-type comets.[15] Halley-type comets, which are named after their prototype, Halley's Comet, are thought to have originated in the Oort cloud but to have been drawn into the inner Solar System by the gravity of the giant planets,[43] whereas the JFCs are thought to have originated in the scattered disc.[19] The centaurs are thought to be a dynamically intermediate stage between the scattered disc and the Jupiter family.[20]

There are many differences between SDOs and JFCs, even though many of the Jupiter-family comets may have originated in the scattered disc. Although the centaurs share a reddish or neutral coloration with many SDOs, their nuclei are bluer, indicating a fundamental chemical or physical difference.[43] One hypothesis is that comet nuclei are resurfaced as they approach the Sun by subsurface materials which subsequently bury the older material.[43]

See also


  1. ^ The literature is inconsistent in the use of the phrases "scattered disc" and "Kuiper belt". For some, they are distinct populations; for others, the scattered disc is part of the Kuiper belt. Authors may even switch between these two uses in a single publication.[3] In this article, the scattered disc will be considered a separate population from the Kuiper belt.


  1. ^ Maggie Masetti. (2007). Cosmic Distance Scales – The Solar System. Website of NASA's High Energy Astrophysics Science Archive Research Center. Retrieved 2008 07-12.
  2. ^ a b Morbidelli, Alessandro (2005). "Origin and dynamical evolution of comets and their reservoirs". arXiv:astro-ph/0512256.
  3. ^ McFadden, Weissman, & Johnson (2007). Encyclopedia of the Solar System, footnote p. 584
  4. ^ Horner, J.; Evans, N. W.; Bailey, Mark E. (2004). "Simulations of the Population of Centaurs I: The Bulk Statistics". Monthly Notices of the Royal Astronomical Society. 354 (3): 798. arXiv:astro-ph/0407400. Bibcode:2004MNRAS.354..798H. doi:10.1111/j.1365-2966.2004.08240.x.
  5. ^ Sheppard, Scott S. (October 16–18, 2005). "Small Bodies in the Outer Solar System" (PDF). New Horizons in Astronomy: Frank N. Bash Symposium 2005. Austin, Texas: Astronomical Society of the Pacific. pp. 3–14. ISBN 1-58381-220-2. Archived from the original (PDF) on 2006-10-12. Retrieved 2008-08-14.
  6. ^ Luu, Jane X.; Marsden, Brian G.; Jewitt, David C. (5 June 1997). "A new dynamical class of object in the outer Solar System" (PDF). Nature. 387 (6633): 573–575. Bibcode:1997Natur.387..573L. doi:10.1038/42413. Archived from the original (PDF) on August 12, 2007. Retrieved 2008-08-02.
  7. ^ Davies, John Keith (2001). Beyond Pluto: Exploring the Outer Limits of the Solar System (PDF). Cambridge University Press. p. 111. ISBN 978-0-521-80019-8. Retrieved 2008-07-02.
  8. ^ a b Jewitt, David C. (August 2009). "Scattered Kuiper Belt Objects (SKBOs)". Institute for Astronomy. Retrieved 2010-01-23.
  9. ^ Schmadel, Lutz D. (2003); Dictionary of Minor Planet Names (5th rev. and enlarged ed. edition). Berlin: Springer. Page 925 (Appendix 10). Also see McFadden, Lucy-Ann; Weissman, Paul & Johnson, Torrence (1999). Encyclopedia of the Solar System. San Diego: Academic Press. Page 218.
  10. ^ a b c IAU: Minor Planet Center (2011-01-03). "List Of Centaurs and Scattered-Disk Objects". Central Bureau for Astronomical Telegrams, Harvard-Smithsonian Center for Astrophysics. Retrieved 2011-01-03.
  11. ^ Schwamb, M. E.; Brown, Michael E.; Rabinowitz, Davdi; Marsden, Brian G. (2008). "2007 UK126". Minor Planet Electronic Circ. 2008-D38: 38. Bibcode:2008MPEC....D...38S.
  12. ^ Staff (2007-05-01). "Discovery Circumstances: Numbered Minor Planets". Minor Planet Center. Retrieved 2010-10-25.
  13. ^ "Discovery Circumstances: Numbered Minor Planets (90001)-(95000)". Minor Planet Center. Retrieved 2010-10-25.
  14. ^ Marc W. Buie (2007-11-08). "Orbit Fit and Astrometric record for 04VN112". SwRI (Space Science Department). Archived from the original on 2010-08-18. Retrieved 2008-07-17.
  15. ^ a b c d e Levison, Harold F.; Donnes, Luke (2007). "Comet Populations and Cometary Dynamics". In Adams McFadden, Lucy Ann; Weissman, Paul Robert; Johnson, Torrence V. (eds.). Encyclopedia of the Solar System (2nd ed.). Amsterdam; Boston: Academic Press. pp. 575–588. ISBN 978-0-12-088589-3. Archived from the original on 2015-09-06.
  16. ^ a b c d e Morbidelli, Alessandro; Brown, Michael E. (2004-11-01). "The Kuiper Belt and the Primordial Evolution of the Solar System" (PDF). In M. C. Festou; H. U. Keller; H. A. Weaver (eds.). Comets II. Tucson (AZ): University of Arizona Press. pp. 175–91. ISBN 978-0-8165-2450-1. OCLC 56755773. Retrieved 2008-07-27.
  17. ^ a b c d e Gomes, Rodney S.; Fernandez, Julio A.; Gallardo, Tabare; Brunini, Adrian (2008). "The Scattered Disk: Origins, Dynamics and End States" (PDF). Universidad de la Republica, Uruguay. Retrieved 2008-08-10.
  18. ^ De Sanctis, M. C.; Capria, M. T.; Coradini, A. (2001). "Thermal Evolution and Differentiation of Edgeworth-Kuiper Belt Objects". The Astronomical Journal. 121 (5): 2792–2799. Bibcode:2001AJ....121.2792D. doi:10.1086/320385.
  19. ^ a b Morbidelli, Alessandro; Levison, Harold F. (2007). "Kuiper Belt Dynamics". In Lucy-Ann Adams McFadden; Paul Robert Weissman; Torrence V. Johnson (eds.). Encyclopedia of the Solar System (2nd ed.). Amsterdam; Boston: Academic Press. pp. 589–604. ISBN 978-0-12-088589-3.
  20. ^ a b Horner, J.; Evans, N. W.; Bailey, Mark E.; Asher, D. J. (2003). "The Populations of Comet-like Bodies in the Solar System". Monthly Notices of the Royal Astronomical Society. 343 (4): 1057–1066. arXiv:astro-ph/0304319. Bibcode:2003MNRAS.343.1057H. doi:10.1046/j.1365-8711.2003.06714.x.
  21. ^ Remo notes that Cis-Neptunian bodies "include terrestrial and large gaseous planets, planetary moons, asteroids, and main-belt comets within Neptune's orbit." (Remo 2007)
  22. ^ Silber, Kenneth (1999). "New Object in Solar System Defies Categories". Archived from the original on September 21, 2005. Retrieved 2008-08-12.
  23. ^ Jewitt, David C. (2008). "The 1000 km Scale KBOs". Retrieved 2010-01-23.
  24. ^ Brown, Michael E. "Sedna (The coldest most distant place known in the solar system; possibly the first object in the long-hypothesized Oort cloud)". California Institute of Technology, Department of Geological Sciences. Retrieved 2008-07-02.
  25. ^ a b Lykawka, Patryk Sofia; Mukai, Tadashi (2007). "Dynamical classification of trans-Neptunian objects: Probing their origin, evolution, and interrelation". Icarus. Kobe. 189 (1): 213–232. Bibcode:2007Icar..189..213L. doi:10.1016/j.icarus.2007.01.001. Archived from the original on 2011-03-10. Retrieved 2008-07-24.
  26. ^ Gladman, Brett J. "Evidence for an Extended Scattered Disk?". Observatoire de la Cote d'Azur. Retrieved 2008-08-02.
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