Classical Kuiper belt object: Difference between revisions

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{{Short description|Kuiper belt object, not controlled by an orbital resonance with Neptune}}
{{Short description|Kuiper belt object, not controlled by an orbital resonance with Neptune}}
[[File:UltimaThule_CA06_color_20190516.png|thumb|[[486958 Arrokoth]], the first classical Kuiper belt object [[List of minor planets visited by spacecraft|visited by a spacecraft]].]]
[[File:UltimaThule_CA06_color_20190516.png|thumb|[[486958 Arrokoth]], the first classical Kuiper belt object [[List of minor planets visited by spacecraft|visited by a spacecraft]].]]
[[File:Cubewanos.png|thumb|The orbits of various cubewanos compared to the orbit of [[Neptune]] (blue) and [[Pluto]] (pink)]]
[[File:Cubewanos.png|thumb|The orbits of various cubewanos compared to the orbit of [[Neptune]] (blue) and [[Pluto]] (magenta)]]
{{TNO}}
{{TNO}}


A '''classical Kuiper belt object''', also called a '''cubewano''' ({{IPAc-en|ˌ|k|juː|b|iː|ˈ|w|ʌ|n|oʊ}} "QB1-o"),{{efn|Somewhat old-fashioned, but "cubewano" is still used by the Minor Planet Center for their list of Distant Minor Planets.<ref>{{cite web |url=http://www.minorplanetcenter.org/mpec/K10/K10S44.html |title=Distant Minor Planets}}</ref>}} is a low-eccentricity [[Kuiper belt]] object (KBO) that [[orbit]]s beyond [[Neptune]] and is not controlled by an [[Resonant trans-Neptunian object|orbital resonance with Neptune]]. Cubewanos have orbits with [[Semi-major axis|semi-major axes]] in the 40–50&nbsp;[[astronomical unit|AU]] range and, unlike [[Pluto]], do not cross Neptune's orbit. That is, they have low-[[Orbital eccentricity|eccentricity]] and sometimes low-[[Orbital inclination|inclination]] orbits like the classical planets.
A '''classical Kuiper belt object''', also called a '''cubewano''' ({{IPAc-en|ˌ|k|juː|b|iː|ˈ|w|ʌ|n|oʊ}} "QB1-o"),{{efn|Somewhat old-fashioned, but "cubewano" is still used by the Minor Planet Center for their list of Distant Minor Planets.<ref>{{cite web |url=http://www.minorplanetcenter.org/mpec/K10/K10S44.html |title=Distant Minor Planets}}</ref>}} is a low-eccentricity [[Kuiper belt]] object (KBO) that [[orbit]]s beyond [[Neptune]] and is not controlled by an [[Resonant trans-Neptunian object|orbital resonance with Neptune]]. Cubewanos have orbits with [[Semi-major axis|semi-major axes]] in the 40–50&nbsp;[[astronomical unit|AU]] range and, unlike [[Pluto]], do not cross Neptune's orbit. That is, they have low-[[Orbital eccentricity|eccentricity]] and sometimes low-[[Orbital inclination|inclination]] orbits like the classical planets.


The name "cubewano" derives from the first [[trans-Neptunian object]] (TNO) found after Pluto and [[Charon (moon)|Charon]]: [[15760 Albion]], which until January 2018 had only the provisional designation (15760) {{mp|1992 QB|1}}.<ref>{{cite web |url=http://www2.ess.ucla.edu/~jewitt/kb/def_classical.html |title=Classical Kuiper Belt Objects |author-link=David Jewitt |first=David |last=Jewitt |publisher=UCLA |access-date=1 July 2013}}</ref> Similar objects found later were often called "QB1-os", or "cubewanos", after this object, though the term "classical" is much more frequently used in the scientific literature.
The name "cubewano" derives from the first [[trans-Neptunian object]] (TNO) found after Pluto and [[Charon (moon)|Charon]]: [[15760 Albion]], which until January 2018 had only the provisional designation (15760) {{mp|1992 QB|1}}.<ref>{{cite web |url=http://www2.ess.ucla.edu/~jewitt/kb/def_classical.html |title=Classical Kuiper Belt Objects |author-link=David C. Jewitt |first=David |last=Jewitt |publisher=UCLA |access-date=1 July 2013}}</ref> Similar objects found later were often called "QB1-os", or "cubewanos", after this object, though the term "classical" is much more frequently used in the scientific literature.


Objects identified as cubewanos include:
Objects identified as cubewanos include:
* [[15760 Albion]]<ref name=K10B62 /> (aka {{mp|1992 QB|1}} and gave rise to term 'Cubewano')
* [[15760 Albion]]<ref name=K10B62 /> (aka {{mp|1992 QB|1}} and gave rise to the term "Cubewano")
* [[Makemake|136472 Makemake]], a [[dwarf planet]]<ref name=K10B62 />  
* [[Makemake]], a [[dwarf planet]]<ref name=K10B62 />  
* [[50000 Quaoar]] and [[20000 Varuna]], each considered the largest TNO at the time of discovery<ref name=K10B62 />  
* [[Quaoar (dwarf planet)|Quaoar]] and [[20000 Varuna]], each considered the largest TNO at the time of discovery<ref name=K10B62 />  
* [[19521 Chaos]], [[58534 Logos]], [[53311 Deucalion]], [[66652 Borasisi]], [[88611 Teharonhiawako]]
* [[19521 Chaos]], [[58534 Logos]], [[53311 Deucalion]], [[66652 Borasisi]], [[88611 Teharonhiawako]]
* {{mpl|(33001) 1997 CU|29}}, {{mpl|(55636) 2002 TX|300}}, [[55565 Aya]], {{mpl|(55637) 2002 UX|25}}
* {{mpl|(33001) 1997 CU|29}}, {{mpl|(55636) 2002 TX|300}}, [[55565 Aya]], [[55637 Uni]]
* [[486958 Arrokoth]]
* [[486958 Arrokoth]]


[[Haumea|136108 Haumea]] was provisionally listed as a cubewano by the [[Minor Planet Center]] in 2006,<ref name=K06X45>{{cite web |date=2006-12-12 |title=MPEC 2006-X45: Distant Minor Planets |url=https://minorplanetcenter.net//mpec/K06/K06X45.html |access-date=2008-10-03 |df=dmy-all |publisher=IAU Minor Planet Center & Tamkin Foundation Computer Network}}</ref> but was later found to be in a [[resonant trans-Neptunian object|resonant]] orbit.<ref name=K10B62>
[[Haumea]] was provisionally listed as a cubewano by the [[Minor Planet Center]] in 2006,<ref name=K06X45>{{cite web |date=2006-12-12 |title=MPEC 2006-X45: Distant Minor Planets |url=https://minorplanetcenter.net//mpec/K06/K06X45.html |access-date=2008-10-03 |df=dmy-all |publisher=IAU Minor Planet Center & Tamkin Foundation Computer Network}}</ref> but was later found to be in a [[resonant trans-Neptunian object|resonant]] orbit.<ref name=K10B62>
{{cite web |date=2010-01-30 |title=MPEC 2010-B62: Distant Minor Planets (2010 FEB. 13.0 TT) |author=Brian G. Marsden |department=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics |url=http://www.minorplanetcenter.org/mpec/K10/K10B62.html |archive-url=https://archive.today/20120904012403/http://www.minorplanetcenter.org/mpec/K10/K10B62.html |url-status=dead |archive-date=2012-09-04 |df=dmy-all |access-date=2010-07-26}}</ref>
{{cite web |date=2010-01-30 |title=MPEC 2010-B62: Distant Minor Planets (2010 FEB. 13.0 TT) |author=Brian G. Marsden |department=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics |url=http://www.minorplanetcenter.org/mpec/K10/K10B62.html |archive-url=https://archive.today/20120904012403/http://www.minorplanetcenter.org/mpec/K10/K10B62.html |url-status=dead |archive-date=2012-09-04 |df=dmy-all |access-date=2010-07-26}}</ref>


== {{vanchor|Orbits 'hot' and 'cold' populations}} ==
== Orbits: 'hot' and 'cold' populations ==
[[File:TheKuiperBelt 55AU Classical.svg|thumb|300px|[[Semimajor axis]] and [[orbital inclination|inclination]] of cubewanos (blue) compared to [[Resonant trans-Neptunian object|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.
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 [[plutino]]s) 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]].
Most cubewanos are found between the 2:3 [[orbital resonance]] with Neptune (populated by [[plutino]]s) 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 (<&thinsp;5[[Degree (angle)|°]]) and near-circular orbits, lying between 42 and 47&nbsp;AU. A smaller population (the ''hot population'') is characterised by highly inclined, more eccentric orbits.<ref name="JewittDelsanti2006">{{cite book |last1=Jewitt |first1=D. |author1-link=David Jewitt |last2=Delsanti |first2=A. |year=2006 |chapter=The Solar System Beyond The Planets |title=Solar System Update : Topical and Timely Reviews in Solar System Sciences |publisher=[[Springer (publisher)|Springer]]-[[Praxis Publishing|Praxis]] |chapter-url=http://www2.ess.ucla.edu/~jewitt/papers/2006/DJ06.pdf |isbn=978-3-540-26056-1 |url=http://www.ifa.hawaii.edu/faculty/jewitt/papers/2006/DJ06.pdf |access-date=March 2, 2006 |archive-url=https://web.archive.org/web/20070129151907/http://www.ifa.hawaii.edu/faculty/jewitt/papers/2006/DJ06.pdf |archive-date=2007-01-29 |df=dmy-all |url-status=dead}})</ref> 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.<ref name="Levison2003">{{cite journal |last1=Levison |first1=Harold F. |last2=Morbidelli |first2=Alessandro |date=2003 |title=The formation of the Kuiper belt by the outward transport of bodies during Neptune's migration |journal=[[Nature (journal)|Nature]] |volume=426 |issue=6965 |pages=419–421 |doi=10.1038/nature02120 |pmid=14647375 |bibcode=2003Natur.426..419L|s2cid=4395099 }}</ref>
The majority of classical objects, the so-called ''cold population'', have low inclinations (< 5[[Degree (angle)|°]]) and near-circular orbits, lying between 42 and 47&nbsp;AU. A smaller population (the ''hot population'') is characterised by highly inclined, more eccentric orbits.<ref name="JewittDelsanti2006">{{cite book |last1=Jewitt |first1=D. |author1-link=David C. Jewitt |last2=Delsanti |first2=A. |year=2006 |chapter=The Solar System Beyond The Planets |title=Solar System Update : Topical and Timely Reviews in Solar System Sciences |publisher=[[Springer (publisher)|Springer]]-[[Praxis Publishing|Praxis]] |chapter-url=http://www2.ess.ucla.edu/~jewitt/papers/2006/DJ06.pdf |isbn=978-3-540-26056-1 |url=http://www.ifa.hawaii.edu/faculty/jewitt/papers/2006/DJ06.pdf |access-date=March 2, 2006 |archive-url=https://web.archive.org/web/20070129151907/http://www.ifa.hawaii.edu/faculty/jewitt/papers/2006/DJ06.pdf |archive-date=2007-01-29 |df=dmy-all |url-status=dead}})</ref> 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.<ref name="Levison2003">{{cite journal |last1=Levison |first1=Harold F. |last2=Morbidelli |first2=Alessandro |date=2003 |title=The formation of the Kuiper belt by the outward transport of bodies during Neptune's migration |journal=[[Nature (journal)|Nature]] |volume=426 |issue=6965 |pages=419–421 |doi=10.1038/nature02120 |pmid=14647375 |bibcode=2003Natur.426..419L|s2cid=4395099 }}</ref>


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'').<ref name="DES_Elliot2006">
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'').<ref name="DES_Elliot2006">
{{cite journal |author=J. L. Elliot |year=2006 |title=The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population |journal=[[Astronomical Journal]] |volume=129 |issue=2 |pages=1117–1162 |bibcode=2005AJ....129.1117E |doi=10.1086/427395 |display-authors=etal|doi-access=free }} ({{cite web |url=http://alpaca.as.arizona.edu/~trilling/des2.pdf |title=Preprint |archive-url=https://web.archive.org/web/20060823112517/http://alpaca.as.arizona.edu/~trilling/des2.pdf |archive-date=2006-08-23 |df=dmy-all}})</ref>
{{cite journal |author=J. L. Elliot |year=2006 |title=The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population |journal=[[Astronomical Journal]] |volume=129 |issue=2 |pages=1117–1162 |bibcode=2005AJ....129.1117E |doi=10.1086/427395 |display-authors=etal|doi-access=free }} ({{cite web |url=http://alpaca.as.arizona.edu/~trilling/des2.pdf |title=Preprint |archive-url=https://web.archive.org/web/20060823112517/http://alpaca.as.arizona.edu/~trilling/des2.pdf |archive-date=2006-08-23 |df=dmy-all}})</ref>
[[File:Kuiper-belt-inclination.svg|thumb|600px|center|[[Semi-major axis]] and [[orbital inclination|inclination]] of Kuiper belt objects, with cold classical KBOs (blue), hot classical KBOs (light blue), [[Plutino|plutinos]] (orange), and [[Resonant trans-Neptunian object|resonant KBOs]] (red). The [[Haumea family]] is additionally highlighted in slate blue.]]


=== Distribution ===
=== Distribution ===
The vast majority of KBOs (more than two-thirds) have inclinations of less than 5° and eccentricities of less than 0.1&nbsp;. 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 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°.
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#Scattered objects versus classical objects|scattered disk objects]].
See also the comparison with [[scattered disk#Scattered objects versus classical objects|scattered disk objects]].


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 <20°. The high inclination of 'hot' cubewanos has not been explained.<ref>
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 <20°. The high inclination of 'hot' cubewanos has not been explained.<ref>
{{cite web |last=Jewitt |first=D. |author-link=David Jewitt |year=2004 |title=Plutino |url=http://www.ifa.hawaii.edu/~jewitt/kb/plutino.html |url-status=dead |archive-url=https://web.archive.org/web/20070419234021/http://www.ifa.hawaii.edu/~jewitt/kb/plutino.html |archive-date=2007-04-19 |df=dmy-all}}</ref>
{{cite web |last=Jewitt |first=D. |author-link=David C. Jewitt |year=2004 |title=Plutino |url=http://www.ifa.hawaii.edu/~jewitt/kb/plutino.html |url-status=dead |archive-url=https://web.archive.org/web/20070419234021/http://www.ifa.hawaii.edu/~jewitt/kb/plutino.html |archive-date=2007-04-19 |df=dmy-all}}</ref>


{{multiple image
{{multiple image
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{{cite journal |author1=A. Doressoundiram |author2=N. Peixinho |author3=C. de Bergh |author4=S. Fornasier |author5=P. Thebault |author6=M. A. Barucci |author7=C. Veillet |title=The Color Distribution in the Edgeworth-Kuiper Belt |journal=The Astronomical Journal |date=October 2002 |arxiv=astro-ph/0206468 |bibcode=2002AJ....124.2279D |doi=10.1086/342447 |volume=124 |issue=4 |page=2279|s2cid=30565926 }}</ref>
{{cite journal |author1=A. Doressoundiram |author2=N. Peixinho |author3=C. de Bergh |author4=S. Fornasier |author5=P. Thebault |author6=M. A. Barucci |author7=C. Veillet |title=The Color Distribution in the Edgeworth-Kuiper Belt |journal=The Astronomical Journal |date=October 2002 |arxiv=astro-ph/0206468 |bibcode=2002AJ....124.2279D |doi=10.1086/342447 |volume=124 |issue=4 |page=2279|s2cid=30565926 }}</ref>
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.<ref name="LacerdaJewitt2008">
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.<ref name="LacerdaJewitt2008">
{{cite journal |first1=Nuno |last1=Peixinho |first2=Pedro |last2=Lacerda |first3=David |last3=Jewitt |author3-link=David Jewitt |title=Color-inclination relation of the classical Kuiper belt objects |journal=The Astronomical Journal |date=August 2008 |arxiv=0808.3025 |bibcode=2008AJ....136.1837P |doi=10.1088/0004-6256/136/5/1837 |volume=136 |issue=5 |pages=1837|s2cid=16473299 }}</ref>
{{cite journal |first1=Nuno |last1=Peixinho |first2=Pedro |last2=Lacerda |first3=David |last3=Jewitt |author3-link=David C. Jewitt |title=Color-inclination relation of the classical Kuiper belt objects |journal=The Astronomical Journal |date=August 2008 |arxiv=0808.3025 |bibcode=2008AJ....136.1837P |doi=10.1088/0004-6256/136/5/1837 |volume=136 |issue=5 |pages=1837|s2cid=16473299 }}</ref>


Another difference between the low-inclination (cold) and high-inclination (hot) classical objects is the observed number of [[binary asteroid|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.<ref name="NollGrundy-binaries2008">
Another difference between the low-inclination (cold) and high-inclination (hot) classical objects is the observed number of [[binary asteroid|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.<ref name="NollGrundy-binaries2008">
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[[File:2014 MU69 orbit.jpg|thumb|New Horizons trajectory and the orbits of Pluto and 486958 Arrokoth]]
[[File:2014 MU69 orbit.jpg|thumb|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 program|Voyager spacecraft]] have passed through the region before the discovery of the Kuiper belt.<ref>{{cite web |url=http://pluto.jhuapl.edu/News-Center/PI-Perspectives.php?page=piPerspective_02_28_2018 |title=The PI's Perspective: Why Didn't Voyager Explore the Kuiper Belt? |date=28 February 2018 |first=Alan |last=Stern |access-date=13 March 2018}}</ref> [[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 {{convert|3500|km|mi}} on 1&nbsp;January 2019.<ref>{{cite web |url=http://www.planetary.org/blogs/emily-lakdawalla/2018/0124-new-horizons-prepares-for-2014mu69.html |title=New Horizons prepares for encounter with 2014&nbsp;MU69 |first=Emily |last=Lakdawalla |publisher=Planetary Society |date=24 January 2018 |access-date=13 March 2018}}</ref>
As of January 2019, only one classical Kuiper belt object has been observed up close by spacecraft. Both [[Voyager program|Voyager spacecraft]] have passed through the region before the discovery of the Kuiper belt.<ref>{{cite web |url=https://pluto.jhuapl.edu/News-Center/PI-Perspectives.php?page=piPerspective_02_28_2018 |title=The PI's Perspective: Why Didn't Voyager Explore the Kuiper Belt? |date=28 February 2018 |first=Alan |last=Stern |access-date=13 March 2018}}</ref> [[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 {{convert|3500|km|mi}} on 1&nbsp;January 2019.<ref>{{cite web |url=https://www.planetary.org/blogs/emily-lakdawalla/2018/0124-new-horizons-prepares-for-2014mu69.html |title=New Horizons prepares for encounter with 2014&nbsp;MU69 |first=Emily |last=Lakdawalla |publisher=Planetary Society |date=24 January 2018 |access-date=13 March 2018}}</ref>


== List ==
== List ==
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* {{mpl|(120178) 2003 OP|32}}
* {{mpl|(120178) 2003 OP|32}}
* [[120347 Salacia]]
* [[120347 Salacia]]
* [[Makemake|136472 Makemake]]
* {{mpl|(144897) 2004 UX|10}}
* {{mpl|(144897) 2004 UX|10}}
* [[145452 Ritona]]
* [[145452 Ritona]]
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* {{mpl|(33001) 1997 CU|29}}
* {{mpl|(33001) 1997 CU|29}}
* [[486958 Arrokoth]]
* [[486958 Arrokoth]]
* [[50000 Quaoar]]
* [[Quaoar (dwarf planet)|50000 Quaoar]]
* {{mpl|(52747) 1998 HM|151}}
* {{mpl|(52747) 1998 HM|151}}
* [[53311 Deucalion]]
* [[53311 Deucalion]]
* [[55565 Aya]]
* [[55565 Aya]]
* {{mpl|(55636) 2002 TX|300}}
* {{mpl|(55636) 2002 TX|300}}
* {{mpl|(55637) 2002 UX|25}}
* [[55637 Uni]]
* [[58534 Logos]]
* [[58534 Logos]]
* [[66652 Borasisi]]
* [[66652 Borasisi]]
Line 140: Line 141:
* {{mpl|(86047) 1999 OY|3}}
* {{mpl|(86047) 1999 OY|3}}
* [[88611 Teharonhiawako]]
* [[88611 Teharonhiawako]]
* {{mpl|(90568) 2004 GV|9}}
* [[90568 Goibniu]]
{{Colend}}
{{Colend}}


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==External links==
==External links==
{{Commonscat|Classical Kuiper belt objects}}
{{Commonscat|Classical Kuiper belt objects}}
*{{cite web |first=David |last=Jewitt |author-link=David Jewitt |url=http://www2.ess.ucla.edu/~jewitt/kb.html |title=Kuiper belt site |publisher=UCLA}}
*{{cite web |first=David |last=Jewitt |author-link=David C. Jewitt |url=http://www2.ess.ucla.edu/~jewitt/kb.html |title=Kuiper belt site |publisher=UCLA}}
*{{cite web |url=http://www.boulder.swri.edu/ekonews/ |title=The Kuiper Belt Electronic Newsletter}}
*{{cite web |url=http://www.boulder.swri.edu/ekonews/ |title=The Kuiper Belt Electronic Newsletter}}
*{{citation |department=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics |url=http://www.minorplanetcenter.org/iau/lists/TNOs.html |website=minorplanetcenter.org |url-status=dead |archive-url=https://web.archive.org/web/20100827234817/http://www.minorplanetcenter.org/iau/lists/TNOs.html |archive-date=2010-08-27 |df=dmy-all |title=List of Trans-Neptunian objects}}
*{{citation |department=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics |url=http://www.minorplanetcenter.org/iau/lists/TNOs.html |website=minorplanetcenter.org |url-status=dead |archive-url=https://web.archive.org/web/20100827234817/http://www.minorplanetcenter.org/iau/lists/TNOs.html |archive-date=2010-08-27 |df=dmy-all |title=List of Trans-Neptunian objects}}
*{{cite web |title=TNO pages |url=http://www.johnstonsarchive.net/astro/tnos.html |website=johnstonarchive.net}}
*{{cite web |title=TNO pages |url=https://www.johnstonsarchive.net/astro/tnos.html |website=johnstonarchive.net}}
*{{cite web |title=Plot of the current positions of bodies in the Outer Solar System |url=http://www.minorplanetcenter.org/iau/lists/OuterPlot.html |website=minorplanetcenter.org |department=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics }}
*{{cite web |title=Plot of the current positions of bodies in the Outer Solar System |url=http://www.minorplanetcenter.org/iau/lists/OuterPlot.html |website=minorplanetcenter.org |department=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics }}


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