fbpx
Wikipedia

Classical Kuiper belt object

December 15, 2023

A classical Kuiper belt object, also called a cubewano (/ˌkjuːbiːˈwʌnoʊ/ "QB1-o"),[a] is a low-eccentricity Kuiper belt object (KBO) that orbits beyond Neptune and is not controlled by an orbital resonance with Neptune. Cubewanos have orbits with semi-major axes in the 40–50 AU range and, unlike Pluto, do not cross Neptune's orbit. That is, they have low-eccentricity and sometimes low-inclination orbits like the classical planets.

486958 Arrokoth, the first classical Kuiper belt object visited by a spacecraft.
The orbits of various cubewanos compared to the orbit of Neptune (blue) and Pluto (pink)

The name "cubewano" derives from the first trans-Neptunian object (TNO) found after Pluto and Charon: 15760 Albion, which until January 2018 had only the provisional designation (15760) 1992 QB1.[2] Similar objects found later were often called "QB1-o's", or "cubewanos", after this object, though the term "classical" is much more frequently used in the scientific literature.

Objects identified as cubewanos include:

136108 Haumea was provisionally listed as a cubewano by the Minor Planet Center in 2006,[4] but was later found to be in a resonant orbit.[3]

Orbits: 'hot' and 'cold' populations edit

 
Semimajor axis and inclination of cubewanos (blue) compared to resonant TNOs (red).

There are two basic dynamical classes of classical Kuiper-belt bodies: those with relatively unperturbed ('cold') orbits, and those with markedly perturbed ('hot') orbits.

Most cubewanos are found between the 2:3 orbital resonance with Neptune (populated by plutinos) and the 1:2 resonance. 50000 Quaoar, for example, has a near-circular orbit close to the ecliptic. Plutinos, on the other hand, have more eccentric orbits bringing some of them closer to the Sun than Neptune.

The majority of classical objects, the so-called cold population, have low inclinations (< 5°) and near-circular orbits, lying between 42 and 47 AU. A smaller population (the hot population) is characterised by highly inclined, more eccentric orbits.[5] The terms 'hot' and 'cold' has nothing to do with surface or internal temperatures, but rather refer to the orbits of the objects, by analogy to molecules in a gas, which increase their relative velocity as they heat up.[6]

The Deep Ecliptic Survey reports the distributions of the two populations; one with the inclination centered at 4.6° (named Core) and another with inclinations extending beyond 30° (Halo).[7]

Distribution edit

The vast majority of KBOs (more than two-thirds) have inclinations of less than 5° and eccentricities of less than 0.1 . Their semi-major axes show a preference for the middle of the main belt; arguably, smaller objects close to the limiting resonances have been either captured into resonance or have their orbits modified by Neptune.

The 'hot' and 'cold' populations are strikingly different: more than 30% of all cubewanos are in low inclination, near-circular orbits. The parameters of the plutinos’ orbits are more evenly distributed, with a local maximum in moderate eccentricities in 0.15–0.2 range, and low inclinations 5–10°. See also the comparison with scattered disk objects.

When the orbital eccentricities of cubewanos and plutinos are compared, it can be seen that the cubewanos form a clear 'belt' outside Neptune's orbit, whereas the plutinos approach, or even cross Neptune's orbit. When orbital inclinations are compared, 'hot' cubewanos can be easily distinguished by their higher inclinations, as the plutinos typically keep orbits below 20°. (No clear explanation currently exists for the inclinations of 'hot' cubewanos.[8])

 
 
Left: TNO distribution of cubewanos (blue), resonant TNOs (red), SDOs (grey) and sednoids (yellow). Right: Comparison of the aligned orbits (polar and ecliptic view) of cubewanos, plutinos, and Neptune (yellow).

Cold and hot populations: physical characteristics edit

In addition to the distinct orbital characteristics, the two populations display different physical characteristics.

The difference in colour between the red cold population, such as 486958 Arrokoth, and more heterogeneous hot population was observed as early as in 2002.[9] Recent studies, based on a larger data set, indicate the cut-off inclination of 12° (instead of 5°) between the cold and hot populations and confirm the distinction between the homogenous red cold population and the bluish hot population.[10]

Another difference between the low-inclination (cold) and high-inclination (hot) classical objects is the observed number of binary objects. Binaries are quite common on low-inclination orbits and are typically similar-brightness systems. Binaries are less common on high-inclination orbits and their components typically differ in brightness. This correlation, together with the differences in colour, support further the suggestion that the currently observed classical objects belong to at least two different overlapping populations, with different physical properties and orbital history.[11]

Toward a formal definition edit

There is no official definition of 'cubewano' or 'classical KBO'. However, the terms are normally used to refer to objects free from significant perturbation from Neptune, thereby excluding KBOs in orbital resonance with Neptune (resonant trans-Neptunian objects). The Minor Planet Center (MPC) and the Deep Ecliptic Survey (DES) do not list cubewanos (classical objects) using the same criteria. Many TNOs classified as cubewanos by the MPC, such as dwarf planet Makemake, are classified as ScatNear (possibly scattered by Neptune) by the DES. (119951) 2002 KX14 may be an inner cubewano near the plutinos. Furthermore, there is evidence that the Kuiper belt has an 'edge', in that an apparent lack of low-inclination objects beyond 47–49 AU was suspected as early as 1998 and shown with more data in 2001.[12] Consequently, the traditional usage of the terms is based on the orbit's semi-major axis, and includes objects situated between the 2:3 and 1:2 resonances, that is between 39.4 and 47.8 AU (with exclusion of these resonances and the minor ones in-between).[5]

These definitions lack precision: in particular the boundary between the classical objects and the scattered disk remains blurred. As of 2023, there are 870 objects with perihelion (q) > 40 AU and aphelion (Q) < 48 AU.[13]

DES classification edit

Introduced by the report from the Deep Ecliptic Survey by J. L. Elliott et al. in 2005 uses formal criteria based on the mean orbital parameters.[7] Put informally, the definition includes the objects that have never crossed the orbit of Neptune. According to this definition, an object qualifies as a classical KBO if:

SSBN07 classification edit

An alternative classification, introduced by B. Gladman, B. Marsden and C. van Laerhoven in 2007, uses a 10-million-year orbit integration instead of the Tisserand's parameter. Classical objects are defined as not resonant and not being currently scattered by Neptune.[14]

Formally, this definition includes as classical all objects with their current orbits that

  • are non-resonant (see the definition of the method)
  • have a semi-major axis greater than that of Neptune (30.1 AU; i.e. excluding centaurs) but less than 2000 AU (to exclude inner-Oort-cloud objects)
  • are not being scattered by Neptune
  • have their eccentricity   (to exclude detached objects)

Unlike other schemes, this definition includes the objects with major semi-axis less than 39.4 AU (2:3 resonance)—termed inner classical belt, or more than 48.7 (1:2 resonance) – termed outer classical belt, and reserves the term main classical belt for the orbits between these two resonances.[14]

Families edit

The first known collisional family in the classical Kuiper belt—a group of objects thought to be remnants from the breakup of a single body—is the Haumea family.[15] It includes Haumea, its moons, 2002 TX300 and seven smaller bodies.† The objects not only follow similar orbits but also share similar physical characteristics. Unlike many other KBO their surface contains large amounts of ice (H2O) and no or very little tholins.[16] The surface composition is inferred from their neutral (as opposed to red) colour and deep absorption at 1.5 and 2. μm in infrared spectrum.[17] Several other collisional families might reside in the classical Kuiper belt.[18][19]

†As of 2008. The four brightest objects of the family are situated on the graphs inside the circle representing Haumea.[clarification needed]

Exploration edit

 
New Horizons trajectory and the orbits of Pluto and 486958 Arrokoth

As of January 2019, only one classical Kuiper belt object has been observed up close by spacecraft. Both Voyager spacecraft have passed through the region before the discovery of the Kuiper belt.[20] New Horizons was the first mission to visit a classical KBO. After its successful exploration of the Pluto system in 2015, the NASA spacecraft has visited the small KBO 486958 Arrokoth at a distance of 3,500 kilometres (2,200 mi) on 1 January 2019.[21]

List edit

For a more comprehensive list, see List of trans-Neptunian objects § List.

Here is a very generic list of classical Kuiper belt objects. As of July 2023, there are about 870 objects with q > 40 AU and Q < 48 AU.[13]

See also edit

Footnotes edit

  1. ^ Somewhat old-fashioned, but “cubewano” is still used by the Minor Planet Center for their list of Distant Minor Planets.[1]

References edit

  1. ^ "Distant Minor Planets".
  2. ^ Jewitt, David. "Classical Kuiper Belt Objects". UCLA. Retrieved 1 July 2013.
  3. ^ a b c d Brian G. Marsden (30 January 2010). "MPEC 2010-B62: Distant Minor Planets (2010 FEB. 13.0 TT)". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. Archived from the original on 4 September 2012. Retrieved 26 July 2010.
  4. ^ "MPEC 2006-X45: Distant Minor Planets". IAU Minor Planet Center & Tamkin Foundation Computer Network. 12 December 2006. Retrieved 3 October 2008.
  5. ^ a b Jewitt, D.; Delsanti, A. (2006). (PDF). Solar System Update : Topical and Timely Reviews in Solar System Sciences (PDF). Springer-Praxis. ISBN 978-3-540-26056-1. Archived from the original (PDF) on 29 January 2007. Retrieved 2 March 2006.)
  6. ^ Levison, Harold F.; Morbidelli, Alessandro (2003). "The formation of the Kuiper belt by the outward transport of bodies during Neptune's migration". Nature. 426 (6965): 419–421. Bibcode:2003Natur.426..419L. doi:10.1038/nature02120. PMID 14647375. S2CID 4395099.
  7. ^ a b J. L. Elliot; et al. (2006). "The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population". Astronomical Journal. 129 (2): 1117–1162. Bibcode:2005AJ....129.1117E. doi:10.1086/427395. ( (PDF). Archived from the original (PDF) on 23 August 2006.)
  8. ^ Jewitt, D. (2004). . Archived from the original on 19 April 2007.
  9. ^ A. Doressoundiram; N. Peixinho; C. de Bergh; S. Fornasier; P. Thebault; M. A. Barucci; C. Veillet (October 2002). "The Color Distribution in the Edgeworth-Kuiper Belt". The Astronomical Journal. 124 (4): 2279. arXiv:astro-ph/0206468. Bibcode:2002AJ....124.2279D. doi:10.1086/342447. S2CID 30565926.
  10. ^ Peixinho, Nuno; Lacerda, Pedro; Jewitt, David (August 2008). "Color-inclination relation of the classical Kuiper belt objects". The Astronomical Journal. 136 (5): 1837. arXiv:0808.3025. Bibcode:2008AJ....136.1837P. doi:10.1088/0004-6256/136/5/1837. S2CID 16473299.
  11. ^ K. Noll; W. Grundy; D. Stephens; H. Levison; S. Kern (April 2008). "Evidence for two populations of classical transneptunian objects: The strong inclination dependence of classical binaries". Icarus. 194 (2): 758. arXiv:0711.1545. Bibcode:2008Icar..194..758N. doi:10.1016/j.icarus.2007.10.022. S2CID 336950.
  12. ^ Trujillo, Chadwick A.; Brown, Michael E. (2001). (PDF). The Astrophysical Journal. 554 (1): L95–L98. Bibcode:2001ApJ...554L..95T. doi:10.1086/320917. S2CID 7982844. Archived from the original (PDF) on 19 September 2006.
  13. ^ a b "q > 40 AU and Q < 48 AU". IAU Minor Planet Center. minorplanetcenter.net. Harvard-Smithsonian Center for Astrophysics. Retrieved 31 July 2023.
  14. ^ a b Gladman, B. J.; Marsden, B.; van Laerhoven, C. (2008). "Nomenclature in the Outer Solar System" (PDF). In Barucci, M. A.; et al. (eds.). The Solar System Beyond Neptune. Tucson: University of Arizona Press. ISBN 978-0-8165-2755-7. (PDF) from the original on 2012-11-02.
  15. ^ Brown, Michael E.; Barkume, Kristina M.; Ragozzine, Darin; Schaller, Emily L. (2007). "A collisional family of icy objects in the Kuiper belt" (PDF). Nature. 446 (7133): 294–6. Bibcode:2007Natur.446..294B. doi:10.1038/nature05619. PMID 17361177. S2CID 4430027. (PDF) from the original on 2018-07-23.
  16. ^ Pinilla-Alonso, N.; Brunetto, R.; Licandro, J.; Gil-Hutton, R.; Roush, T. L.; Strazzulla, G. (2009). "The surface of (136108) Haumea (2003 EL61), the largest carbon-depleted object in the trans-Neptunian belt". Astronomy and Astrophysics. 496 (2): 547. arXiv:0803.1080. Bibcode:2009A&A...496..547P. doi:10.1051/0004-6361/200809733. S2CID 15139257.
  17. ^ Pinilla-Alonso, N.; Licandro, J.; Gil-Hutton, R.; Brunetto, R. (2007). "The water ice rich surface of (145453) 2005 RR43: a case for a carbon-depleted population of TNOs?". Astronomy and Astrophysics. 468 (1): L25–L28. arXiv:astro-ph/0703098. Bibcode:2007A&A...468L..25P. doi:10.1051/0004-6361:20077294. S2CID 18546361.
  18. ^ Chiang, E.-I. (July 2002). "A Collisional Family in the Classical Kuiper Belt". The Astrophysical Journal. 573 (1): L65–L68. arXiv:astro-ph/0205275. Bibcode:2002ApJ...573L..65C. doi:10.1086/342089. S2CID 18671789.
  19. ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (11 February 2018). "Dynamically correlated minor bodies in the outer Solar system". Monthly Notices of the Royal Astronomical Society. 474 (1): 838–846. arXiv:1710.07610. Bibcode:2018MNRAS.474..838D. doi:10.1093/mnras/stx2765. S2CID 73588205.
  20. ^ Stern, Alan (28 February 2018). "The PI's Perspective: Why Didn't Voyager Explore the Kuiper Belt?". Retrieved 13 March 2018.
  21. ^ Lakdawalla, Emily (24 January 2018). "New Horizons prepares for encounter with 2014 MU69". Planetary Society. Retrieved 13 March 2018.

External links edit

 
Wikimedia Commons has media related to Classical Kuiper belt objects.
  • Jewitt, David. "Kuiper belt site". UCLA.
  • "The Kuiper Belt Electronic Newsletter".
  • , IAU Minor Planet Center, minorplanetcenter.org, Harvard-Smithsonian Center for Astrophysics, archived from the original on 27 August 2010
  • "TNO pages". johnstonarchive.net.
  • "Plot of the current positions of bodies in the Outer Solar System". IAU Minor Planet Center. minorplanetcenter.org. Harvard-Smithsonian Center for Astrophysics.

December 15, 2023
classical, kuiper, belt, object, classical, kuiper, belt, object, also, called, cubewano, juː, eccentricity, kuiper, belt, object, that, orbits, beyond, neptune, controlled, orbital, resonance, with, neptune, cubewanos, have, orbits, with, semi, major, axes, r. A classical Kuiper belt object also called a cubewano ˌ k juː b iː ˈ w ʌ n oʊ QB1 o a is a low eccentricity Kuiper belt object KBO that orbits beyond Neptune and is not controlled by an orbital resonance with Neptune Cubewanos have orbits with semi major axes in the 40 50 AU range and unlike Pluto do not cross Neptune s orbit That is they have low eccentricity and sometimes low inclination orbits like the classical planets 486958 Arrokoth the first classical Kuiper belt object visited by a spacecraft The orbits of various cubewanos compared to the orbit of Neptune blue and Pluto pink The name cubewano derives from the first trans Neptunian object TNO found after Pluto and Charon 15760 Albion which until January 2018 had only the provisional designation 15760 1992 QB1 2 Similar objects found later were often called QB1 o s or cubewanos after this object though the term classical is much more frequently used in the scientific literature Objects identified as cubewanos include 15760 Albion 3 aka 1992 QB1 and gave rise to term Cubewano 136472 Makemake the largest known cubewano and a dwarf planet 3 50000 Quaoar and 20000 Varuna each considered the largest TNO at the time of discovery 3 19521 Chaos 58534 Logos 53311 Deucalion 66652 Borasisi 88611 Teharonhiawako 33001 1997 CU29 55636 2002 TX300 55565 2002 AW197 55637 2002 UX25 486958 Arrokoth136108 Haumea was provisionally listed as a cubewano by the Minor Planet Center in 2006 4 but was later found to be in a resonant orbit 3 Contents 1 Orbits hot and cold populations 1 1 Distribution 2 Cold and hot populations physical characteristics 3 Toward a formal definition 3 1 DES classification 3 2 SSBN07 classification 4 Families 5 Exploration 6 List 7 See also 8 Footnotes 9 References 10 External linksOrbits hot and cold populations edit nbsp Semimajor axis and inclination of cubewanos blue compared to resonant TNOs red There are two basic dynamical classes of classical Kuiper belt bodies those with relatively unperturbed cold orbits and those with markedly perturbed hot orbits Most cubewanos are found between the 2 3 orbital resonance with Neptune populated by plutinos and the 1 2 resonance 50000 Quaoar for example has a near circular orbit close to the ecliptic Plutinos on the other hand have more eccentric orbits bringing some of them closer to the Sun than Neptune The majority of classical objects the so called cold population have low inclinations lt 5 and near circular orbits lying between 42 and 47 AU A smaller population the hot population is characterised by highly inclined more eccentric orbits 5 The terms hot and cold has nothing to do with surface or internal temperatures but rather refer to the orbits of the objects by analogy to molecules in a gas which increase their relative velocity as they heat up 6 The Deep Ecliptic Survey reports the distributions of the two populations one with the inclination centered at 4 6 named Core and another with inclinations extending beyond 30 Halo 7 Distribution edit The vast majority of KBOs more than two thirds have inclinations of less than 5 and eccentricities of less than 0 1 Their semi major axes show a preference for the middle of the main belt arguably smaller objects close to the limiting resonances have been either captured into resonance or have their orbits modified by Neptune The hot and cold populations are strikingly different more than 30 of all cubewanos are in low inclination near circular orbits The parameters of the plutinos orbits are more evenly distributed with a local maximum in moderate eccentricities in 0 15 0 2 range and low inclinations 5 10 See also the comparison with scattered disk objects When the orbital eccentricities of cubewanos and plutinos are compared it can be seen that the cubewanos form a clear belt outside Neptune s orbit whereas the plutinos approach or even cross Neptune s orbit When orbital inclinations are compared hot cubewanos can be easily distinguished by their higher inclinations as the plutinos typically keep orbits below 20 No clear explanation currently exists for the inclinations of hot cubewanos 8 nbsp nbsp Left TNO distribution of cubewanos blue resonant TNOs red SDOs grey and sednoids yellow Right Comparison of the aligned orbits polar and ecliptic view of cubewanos plutinos and Neptune yellow Cold and hot populations physical characteristics editIn addition to the distinct orbital characteristics the two populations display different physical characteristics The difference in colour between the red cold population such as 486958 Arrokoth and more heterogeneous hot population was observed as early as in 2002 9 Recent studies based on a larger data set indicate the cut off inclination of 12 instead of 5 between the cold and hot populations and confirm the distinction between the homogenous red cold population and the bluish hot population 10 Another difference between the low inclination cold and high inclination hot classical objects is the observed number of binary objects Binaries are quite common on low inclination orbits and are typically similar brightness systems Binaries are less common on high inclination orbits and their components typically differ in brightness This correlation together with the differences in colour support further the suggestion that the currently observed classical objects belong to at least two different overlapping populations with different physical properties and orbital history 11 Toward a formal definition editThere is no official definition of cubewano or classical KBO However the terms are normally used to refer to objects free from significant perturbation from Neptune thereby excluding KBOs in orbital resonance with Neptune resonant trans Neptunian objects The Minor Planet Center MPC and the Deep Ecliptic Survey DES do not list cubewanos classical objects using the same criteria Many TNOs classified as cubewanos by the MPC such as dwarf planet Makemake are classified as ScatNear possibly scattered by Neptune by the DES 119951 2002 KX14 may be an inner cubewano near the plutinos Furthermore there is evidence that the Kuiper belt has an edge in that an apparent lack of low inclination objects beyond 47 49 AU was suspected as early as 1998 and shown with more data in 2001 12 Consequently the traditional usage of the terms is based on the orbit s semi major axis and includes objects situated between the 2 3 and 1 2 resonances that is between 39 4 and 47 8 AU with exclusion of these resonances and the minor ones in between 5 These definitions lack precision in particular the boundary between the classical objects and the scattered disk remains blurred As of 2023 update there are 870 objects with perihelion q gt 40 AU and aphelion Q lt 48 AU 13 DES classification edit Introduced by the report from the Deep Ecliptic Survey by J L Elliott et al in 2005 uses formal criteria based on the mean orbital parameters 7 Put informally the definition includes the objects that have never crossed the orbit of Neptune According to this definition an object qualifies as a classical KBO if it is not resonant its average Tisserand s parameter with respect to Neptune exceeds 3 its average eccentricity is less than 0 2 SSBN07 classification edit An alternative classification introduced by B Gladman B Marsden and C van Laerhoven in 2007 uses a 10 million year orbit integration instead of the Tisserand s parameter Classical objects are defined as not resonant and not being currently scattered by Neptune 14 Formally this definition includes as classical all objects with their current orbits that are non resonant see the definition of the method have a semi major axis greater than that of Neptune 30 1 AU i e excluding centaurs but less than 2000 AU to exclude inner Oort cloud objects are not being scattered by Neptune have their eccentricity e lt 0 240 displaystyle e lt 0 240 nbsp to exclude detached objects Unlike other schemes this definition includes the objects with major semi axis less than 39 4 AU 2 3 resonance termed inner classical belt or more than 48 7 1 2 resonance termed outer classical belt and reserves the term main classical belt for the orbits between these two resonances 14 Families editThe first known collisional family in the classical Kuiper belt a group of objects thought to be remnants from the breakup of a single body is the Haumea family 15 It includes Haumea its moons 2002 TX300 and seven smaller bodies The objects not only follow similar orbits but also share similar physical characteristics Unlike many other KBO their surface contains large amounts of ice H2O and no or very little tholins 16 The surface composition is inferred from their neutral as opposed to red colour and deep absorption at 1 5 and 2 mm in infrared spectrum 17 Several other collisional families might reside in the classical Kuiper belt 18 19 As of 2008 The four brightest objects of the family are situated on the graphs inside the circle representing Haumea clarification needed Exploration edit nbsp New Horizons trajectory and the orbits of Pluto and 486958 ArrokothAs of January 2019 only one classical Kuiper belt object has been observed up close by spacecraft Both Voyager spacecraft have passed through the region before the discovery of the Kuiper belt 20 New Horizons was the first mission to visit a classical KBO After its successful exploration of the Pluto system in 2015 the NASA spacecraft has visited the small KBO 486958 Arrokoth at a distance of 3 500 kilometres 2 200 mi on 1 January 2019 21 List editFor a more comprehensive list see List of trans Neptunian objects List Here is a very generic list of classical Kuiper belt objects As of July 2023 update there are about 870 objects with q gt 40 AU and Q lt 48 AU 13 15760 Albion 20000 Varuna 307261 2002 MS4 307616 2003 QW90 444030 2004 NT33 308193 2005 CB79 119951 2002 KX14 120178 2003 OP32 120347 Salacia 144897 2004 UX10 145452 2005 RN43 145453 2005 RR43 148780 Altjira 15807 1994 GV9 16684 1994 JQ1 174567 Varda 19255 1994 VK8 19521 Chaos 202421 2005 UQ513 24835 1995 SM55 24978 1998 HJ151 278361 2007 JJ43 33001 1997 CU29 486958 Arrokoth 50000 Quaoar 52747 1998 HM151 53311 Deucalion 55565 2002 AW197 55636 2002 TX300 55637 2002 UX25 58534 Logos 66652 Borasisi 69987 1998 WA25 79360 Sila Nunam 79983 1999 DF9 85627 1998 HP151 85633 1998 KR65 86047 1999 OY3 88611 Teharonhiawako 90568 2004 GV9See also editLists of astronomical objectsFootnotes edit Somewhat old fashioned but cubewano is still used by the Minor Planet Center for their list of Distant Minor Planets 1 References edit Distant Minor Planets Jewitt David Classical Kuiper Belt Objects UCLA Retrieved 1 July 2013 a b c d Brian G Marsden 30 January 2010 MPEC 2010 B62 Distant Minor Planets 2010 FEB 13 0 TT IAU Minor Planet Center Harvard Smithsonian Center for Astrophysics Archived from the original on 4 September 2012 Retrieved 26 July 2010 MPEC 2006 X45 Distant Minor Planets IAU Minor Planet Center amp Tamkin Foundation Computer Network 12 December 2006 Retrieved 3 October 2008 a b Jewitt D Delsanti A 2006 The Solar System Beyond The Planets PDF Solar System Update Topical and Timely Reviews in Solar System Sciences PDF Springer Praxis ISBN 978 3 540 26056 1 Archived from the original PDF on 29 January 2007 Retrieved 2 March 2006 Levison Harold F Morbidelli Alessandro 2003 The formation of the Kuiper belt by the outward transport of bodies during Neptune s migration Nature 426 6965 419 421 Bibcode 2003Natur 426 419L doi 10 1038 nature02120 PMID 14647375 S2CID 4395099 a b J L Elliot et al 2006 The Deep Ecliptic Survey A Search for Kuiper Belt Objects and Centaurs II Dynamical Classification the Kuiper Belt Plane and the Core Population Astronomical Journal 129 2 1117 1162 Bibcode 2005AJ 129 1117E doi 10 1086 427395 Preprint PDF Archived from the original PDF on 23 August 2006 Jewitt D 2004 Plutino Archived from the original on 19 April 2007 A Doressoundiram N Peixinho C de Bergh S Fornasier P Thebault M A Barucci C Veillet October 2002 The Color Distribution in the Edgeworth Kuiper Belt The Astronomical Journal 124 4 2279 arXiv astro ph 0206468 Bibcode 2002AJ 124 2279D doi 10 1086 342447 S2CID 30565926 Peixinho Nuno Lacerda Pedro Jewitt David August 2008 Color inclination relation of the classical Kuiper belt objects The Astronomical Journal 136 5 1837 arXiv 0808 3025 Bibcode 2008AJ 136 1837P doi 10 1088 0004 6256 136 5 1837 S2CID 16473299 K Noll W Grundy D Stephens H Levison S Kern April 2008 Evidence for two populations of classical transneptunian objects The strong inclination dependence of classical binaries Icarus 194 2 758 arXiv 0711 1545 Bibcode 2008Icar 194 758N doi 10 1016 j icarus 2007 10 022 S2CID 336950 Trujillo Chadwick A Brown Michael E 2001 The Radial Distribution of the Kuiper Belt PDF The Astrophysical Journal 554 1 L95 L98 Bibcode 2001ApJ 554L 95T doi 10 1086 320917 S2CID 7982844 Archived from the original PDF on 19 September 2006 a b q gt 40 AU and Q lt 48 AU IAU Minor Planet Center minorplanetcenter net Harvard Smithsonian Center for Astrophysics Retrieved 31 July 2023 a b Gladman B J Marsden B van Laerhoven C 2008 Nomenclature in the Outer Solar System PDF In Barucci M A et al eds The Solar System Beyond Neptune Tucson University of Arizona Press ISBN 978 0 8165 2755 7 Archived PDF from the original on 2012 11 02 Brown Michael E Barkume Kristina M Ragozzine Darin Schaller Emily L 2007 A collisional family of icy objects in the Kuiper belt PDF Nature 446 7133 294 6 Bibcode 2007Natur 446 294B doi 10 1038 nature05619 PMID 17361177 S2CID 4430027 Archived PDF from the original on 2018 07 23 Pinilla Alonso N Brunetto R Licandro J Gil Hutton R Roush T L Strazzulla G 2009 The surface of 136108 Haumea 2003 EL61 the largest carbon depleted object in the trans Neptunian belt Astronomy and Astrophysics 496 2 547 arXiv 0803 1080 Bibcode 2009A amp A 496 547P doi 10 1051 0004 6361 200809733 S2CID 15139257 Pinilla Alonso N Licandro J Gil Hutton R Brunetto R 2007 The water ice rich surface of 145453 2005 RR43 a case for a carbon depleted population of TNOs Astronomy and Astrophysics 468 1 L25 L28 arXiv astro ph 0703098 Bibcode 2007A amp A 468L 25P doi 10 1051 0004 6361 20077294 S2CID 18546361 Chiang E I July 2002 A Collisional Family in the Classical Kuiper Belt The Astrophysical Journal 573 1 L65 L68 arXiv astro ph 0205275 Bibcode 2002ApJ 573L 65C doi 10 1086 342089 S2CID 18671789 de la Fuente Marcos Carlos de la Fuente Marcos Raul 11 February 2018 Dynamically correlated minor bodies in the outer Solar system Monthly Notices of the Royal Astronomical Society 474 1 838 846 arXiv 1710 07610 Bibcode 2018MNRAS 474 838D doi 10 1093 mnras stx2765 S2CID 73588205 Stern Alan 28 February 2018 The PI s Perspective Why Didn t Voyager Explore the Kuiper Belt Retrieved 13 March 2018 Lakdawalla Emily 24 January 2018 New Horizons prepares for encounter with 2014 MU69 Planetary Society Retrieved 13 March 2018 External links edit nbsp Wikimedia Commons has media related to Classical Kuiper belt objects Jewitt David Kuiper belt site UCLA The Kuiper Belt Electronic Newsletter List of Trans Neptunian objects IAU Minor Planet Center minorplanetcenter org Harvard Smithsonian Center for Astrophysics archived from the original on 27 August 2010 TNO pages johnstonarchive net Plot of the current positions of bodies in the Outer Solar System IAU Minor Planet Center minorplanetcenter org Harvard Smithsonian Center for Astrophysics Portals nbsp Astronomy nbsp Spaceflight nbsp Outer space nbsp Solar System Retrieved from https en wikipedia org w index php title Classical Kuiper belt object amp oldid 1183391066, wikipedia, wiki, book, books, library,

article

, read, download, free, free download, mp3, video, mp4, 3gp, jpg, jpeg, gif, png, picture, music, song, movie, book, game, games.