Plutino: Difference between revisions
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{{about-distinguish-text|the dynamical group|[[plutoid]]s or [[pluton]]s}} | {{about-distinguish-text|the dynamical group|[[plutoid]]s or [[pluton]]s}} | ||
In [[astronomy]], the '''plutinos''' are a [[List of minor-planet groups|dynamical group]] of [[trans-Neptunian object]]s that orbit in 2:3 [[orbital resonance|mean-motion resonance]] with [[Neptune]]. This means that for every two orbits a plutino makes, Neptune orbits three times. The dwarf planet [[Pluto]] is the largest member as well as the namesake of this group. The next largest members are {{dp|Orcus}}, | In [[astronomy]], the '''plutinos''' are a [[List of minor-planet groups|dynamical group]] of [[trans-Neptunian object]]s that orbit in 2:3 [[orbital resonance|mean-motion resonance]] with [[Neptune]]. This means that for every two orbits a plutino makes, Neptune orbits three times. The dwarf planet [[Pluto]] is the largest member as well as the namesake of this group. The next largest members are {{dp|Orcus}}, [[208996 Achlys|Achlys]], and {{dp|Ixion}}. Plutinos [[Astronomical naming conventions#Minor planets|are named after]] mythological creatures associated with the underworld. | ||
Plutinos form the inner part of the [[Kuiper belt]] and represent about a quarter of the known [[Kuiper belt object]]s. They are also the most populous known class of [[resonant trans-Neptunian object]]s ''(also see adjunct box with hierarchical listing)''. The first plutino after Pluto itself, [[(385185) 1993 RO]], was discovered on September 16, 1993. | Plutinos form the inner part of the [[Kuiper belt]] and represent about a quarter of the known [[Kuiper belt object]]s. They are also the most populous known class of [[resonant trans-Neptunian object]]s ''(also see adjunct box with hierarchical listing)''. The first plutino after Pluto itself, [[(385185) 1993 RO]], was discovered on September 16, 1993. | ||
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=== Origin === | === Origin === | ||
It is thought that the objects that are currently in mean [[orbital resonance]]s with Neptune initially followed a variety of independent heliocentric paths. As Neptune migrated outward early in the Solar System's history (see [[Kuiper belt#Origin|origins of the Kuiper belt]]), the bodies it approached would have been scattered; during this process, some of them would have been captured into resonances.<ref name="Malhotra1995">{{cite journal |last1=Malhotra |title=The Origin of Pluto's Orbit: Implications for the Solar System Beyond Neptune |journal=Astronomical Journal |volume=110 |year=1995 |page=420 |arxiv = astro-ph/9504036 |bibcode = 1995AJ....110..420M |doi = 10.1086/117532 |first1= Renu|s2cid= 10622344}}</ref> The 3:2 resonance is a low-order resonance and is thus the strongest and most stable among all resonances.<ref>{{cite journal|last1=Almeida|first1=A.J.C|last2=Peixinho|first2=N.|last3=Correia|first3=A.C.M. |url=https://www.researchgate.net/publication/45876510|title=Neptune Trojans & Plutinos: Colors, sizes, dynamics, & their possible collisions|date=December 2009|journal=Astronomy & Astrophysics|doi=10.1051/0004-6361/200911943|volume=508|issue=2|pages=1021–1030|access-date=2019-07-20|arxiv=0910.0865|s2cid=53772214}}</ref> This is the primary reason it has a larger population than the other Neptunian resonances encountered in the Kuiper Belt. The cloud of low-inclination bodies beyond 40 [[Astronomical unit|AU]] is the [[Classical Kuiper belt object|cubewano]] family, while bodies with higher [[Orbital eccentricity|eccentricities]] (0.05 to 0.34) and [[Semi-major and semi-minor axes| | It is thought that the objects that are currently in mean [[orbital resonance]]s with Neptune initially followed a variety of independent heliocentric paths. As Neptune migrated outward early in the Solar System's history (see [[Kuiper belt#Origin|origins of the Kuiper belt]]), the bodies it approached would have been scattered; during this process, some of them would have been captured into resonances.<ref name="Malhotra1995">{{cite journal |last1=Malhotra |title=The Origin of Pluto's Orbit: Implications for the Solar System Beyond Neptune |journal=Astronomical Journal |volume=110 |year=1995 |page=420 |arxiv = astro-ph/9504036 |bibcode = 1995AJ....110..420M |doi = 10.1086/117532 |first1= Renu|s2cid= 10622344}}</ref> The 3:2 resonance is a low-order resonance and is thus the strongest and most stable among all resonances.<ref>{{cite journal|last1=Almeida|first1=A.J.C|last2=Peixinho|first2=N.|last3=Correia|first3=A.C.M. |url=https://www.researchgate.net/publication/45876510|title=Neptune Trojans & Plutinos: Colors, sizes, dynamics, & their possible collisions|date=December 2009|journal=Astronomy & Astrophysics|doi=10.1051/0004-6361/200911943|volume=508|issue=2|pages=1021–1030|access-date=2019-07-20|arxiv=0910.0865|s2cid=53772214}}</ref> This is the primary reason it has a larger population than the other Neptunian resonances encountered in the Kuiper Belt. The cloud of low-inclination bodies beyond 40 [[Astronomical unit|AU]] is the [[Classical Kuiper belt object|cubewano]] family, while bodies with higher [[Orbital eccentricity|eccentricities]] (0.05 to 0.34) and [[Semi-major and semi-minor axes|semi-major axes]] close to the 3:2 Neptune resonance are primarily plutinos.<ref>{{cite book|url=https://books.google.com/books?id=QpcKesJwp28C&pg=PA411|first=John S.|publisher=Academic Press|department=Centaurs & Trans-Neptunian Objects|last=Lewis|isbn=012446744X |title=Physics & Chemistry of the Solar System|date=2004|pages=409–412|access-date=2019-07-21}}</ref> | ||
=== Orbital characteristics === | === Orbital characteristics === | ||
[[File:Plutino distributions and sizes.png|thumb|The distribution of Plutinos, and relative sizes, drawn 1 million times larger.]] | [[File:Plutino distributions and sizes.png|thumb|The distribution of Plutinos, and relative sizes, drawn 1 million times larger.]] | ||
While the majority of plutinos have relatively low [[orbital inclination]]s, a significant fraction of these objects follow orbits similar to that of Pluto, with inclinations in the 10–25° range and eccentricities around 0.2–0.25; such orbits result in many of these objects having [[perihelion|perihelia]] close to or even inside Neptune's orbit, while simultaneously having [[aphelion|aphelia]] that bring them close to the main [[Kuiper belt]]'s outer edge (where objects in a 1:2 resonance with Neptune, the | While the majority of plutinos have relatively low [[orbital inclination]]s, a significant fraction of these objects follow orbits similar to that of Pluto, with inclinations in the 10–25° range and eccentricities around 0.2–0.25; such orbits result in many of these objects having [[perihelion|perihelia]] close to or even inside Neptune's orbit, while simultaneously having [[aphelion|aphelia]] that bring them close to the main [[Kuiper belt]]'s outer edge (where objects in a 1:2 resonance with Neptune, the twotinos, are found). | ||
The orbital periods of plutinos cluster around 247.3 years (1.5 × Neptune's orbital period), varying by at most a few years from this value. | The orbital periods of plutinos cluster around 247.3 years (1.5 × Neptune's orbital period), varying by at most a few years from this value. | ||
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| issue=2 | pages=700–705 | year=2001 | | issue=2 | pages=700–705 | year=2001 | ||
| bibcode=2001A&A...368..700W| doi = 10.1051/0004-6361:20010056 | | bibcode=2001A&A...368..700W| doi = 10.1051/0004-6361:20010056 | ||
| doi-access=free}}</ref> Numerical simulations suggest that the orbits of plutinos with an eccentricity 10%–30% smaller or larger than that of Pluto are not stable over | | doi-access=free}}</ref> Numerical simulations suggest that the orbits of plutinos with an eccentricity 10%–30% smaller or larger than that of Pluto are not stable over billion-year timescales.<ref name="Yu1999">{{cite journal |first1=Qingjuan |last1=Yu |first2=Scott |last2=Tremaine |title=The Dynamics of Plutinos |journal=Astronomical Journal |volume=118 |year=1999 |issue= 4|pages=1873–1881 |arxiv = astro-ph/9904424 |bibcode = 1999AJ....118.1873Y |doi = 10.1086/301045 |s2cid=14482507 }}</ref> | ||
== Orbital diagrams == | == Orbital diagrams == | ||
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| [[90482 Orcus]] || 39.2 || 30.3 || 20.6 || data-sort-value="2.3"|{{val|2.31|0.03}} || data-sort-value="917"|{{val|917|25}} || {{val|6.32|0.05}} || {{val|0.28|0.06}} || 0.37 || 2004 || M. Brown,<br />C. Trujillo,<br />D. Rabinowitz || {{JPL|90482}} | | [[90482 Orcus]] || 39.2 || 30.3 || 20.6 || data-sort-value="2.3"|{{val|2.31|0.03}} || data-sort-value="917"|{{val|917|25}} || {{val|6.32|0.05}} || {{val|0.28|0.06}} || 0.37 || 2004 || M. Brown,<br />C. Trujillo,<br />D. Rabinowitz || {{JPL|90482}} | ||
|- | |- | ||
| | | [[208996 Achlys]] || 39.4 || 32.3 || 13.6 || data-sort-value="3.7"|{{val|3.74|0.08}} || data-sort-value="717"|{{val|727.0|+61.9|-66.5}} || ≈ 3 || {{val|0.107|+0.023|-0.016}} || {{val|0.38|0.04}} || 2003 || M. Brown,<br />C. Trujillo || {{JPL|208996}} | ||
|- | |- | ||
| [[28978 Ixion]] || 39.7 || 30.1 || 19.6 || data-sort-value="3.8"|{{val|3.828|0.039}} || data-sort-value="617"|{{val|617|19|20}} || ≈ 3 || {{val|0.141|0.011}} || 0.61 || 2001 || [[Deep Ecliptic Survey]] || {{JPL|28978}} | | [[28978 Ixion]] || 39.7 || 30.1 || 19.6 || data-sort-value="3.8"|{{val|3.828|0.039}} || data-sort-value="617"|{{val|617|19|20}} || ≈ 3 || {{val|0.141|0.011}} || 0.61 || 2001 || [[Deep Ecliptic Survey]] || {{JPL|28978}} | ||
Latest revision as of 21:08, 8 November 2025
Template:Short description Template:About-distinguish-text
In astronomy, the plutinos are a dynamical group of trans-Neptunian objects that orbit in 2:3 mean-motion resonance with Neptune. This means that for every two orbits a plutino makes, Neptune orbits three times. The dwarf planet Pluto is the largest member as well as the namesake of this group. The next largest members are Template:Dp, Achlys, and Template:Dp. Plutinos are named after mythological creatures associated with the underworld.
Plutinos form the inner part of the Kuiper belt and represent about a quarter of the known Kuiper belt objects. They are also the most populous known class of resonant trans-Neptunian objects (also see adjunct box with hierarchical listing). The first plutino after Pluto itself, (385185) 1993 RO, was discovered on September 16, 1993.
Orbits
Origin
It is thought that the objects that are currently in mean orbital resonances with Neptune initially followed a variety of independent heliocentric paths. As Neptune migrated outward early in the Solar System's history (see origins of the Kuiper belt), the bodies it approached would have been scattered; during this process, some of them would have been captured into resonances.[1] The 3:2 resonance is a low-order resonance and is thus the strongest and most stable among all resonances.[2] This is the primary reason it has a larger population than the other Neptunian resonances encountered in the Kuiper Belt. The cloud of low-inclination bodies beyond 40 AU is the cubewano family, while bodies with higher eccentricities (0.05 to 0.34) and semi-major axes close to the 3:2 Neptune resonance are primarily plutinos.[3]
Orbital characteristics
While the majority of plutinos have relatively low orbital inclinations, a significant fraction of these objects follow orbits similar to that of Pluto, with inclinations in the 10–25° range and eccentricities around 0.2–0.25; such orbits result in many of these objects having perihelia close to or even inside Neptune's orbit, while simultaneously having aphelia that bring them close to the main Kuiper belt's outer edge (where objects in a 1:2 resonance with Neptune, the twotinos, are found).
The orbital periods of plutinos cluster around 247.3 years (1.5 × Neptune's orbital period), varying by at most a few years from this value.
Unusual plutinos include:
- [[List of unnumbered trans-Neptunian objects: 2005#2005 TV189|Template:Mp]], which follows the most highly inclined orbit (34.5°)
- Template:Mpl, which has the most elliptical orbit (its eccentricity is 0.33), with the perihelion halfway between Uranus and Neptune
- Template:Mpl following a quasi-circular orbit
- [[List of unnumbered trans-Neptunian objects: 2002#2002 VX130|Template:Mp]] lying almost perfectly on the ecliptic (inclination less than 1.5°)
- 15810 Arawn, a quasi-satellite of Pluto[4]
See also the comparison with the distribution of the cubewanos.
Long-term stability
Pluto's influence on the other plutinos has historically been neglected due to its relatively small mass. However, the resonance width (the range of semi-axes compatible with the resonance) is very narrow and only a few times larger than Pluto's Hill sphere (gravitational influence). Consequently, depending on the original eccentricity, some plutinos will eventually be driven out of the resonance by interactions with Pluto.[5] Numerical simulations suggest that the orbits of plutinos with an eccentricity 10%–30% smaller or larger than that of Pluto are not stable over billion-year timescales.[6]
Orbital diagrams
-
The motions of Orcus and Pluto in a rotating frame with a period equal to Neptune's orbital period (holding Neptune stationary). Pluto is grey, Orcus is red, and Neptune is the white (stationary) dot at 5 o'clock. Uranus is blue, Saturn yellow, and Jupiter red.
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Orbits and sizes of the larger plutinos (and the reference non-plutino Template:Mpl-). Orbital eccentricity is represented by segments extending horizontally from perihelion to aphelion; inclination is shown on the vertical axis.
-
The distribution of plutinos (and the reference non-plutino Template:Mp). Small inserts show histograms for the distributions of orbital inclination and eccentricity.
Brightest objects
The plutinos brighter than HV=6 include:
(link to all of the orbits of these objects listed above are here)
See also
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References
Template:Reflist Template:Refbegin
- D.Jewitt, A.Delsanti The Solar System Beyond The Planets in Solar System Update : Topical and Timely Reviews in Solar System Sciences , Springer-Praxis Ed., Template:ISBN (2006). Preprint of the article (pdf)
- Bernstein G.M., Trilling D.E., Allen R.L., Brown K.E, Holman M., Malhotra R. The size Distribution of transneptunian bodies. The Astronomical Journal, 128, 1364–1390. preprint on arXiv
- Minor Planet Center Orbit database (MPCORB) as of 2008-10-05.
- Minor Planet Circular 2008-S05 (October 2008) Distant Minor planets was used for orbit classification.
External links
Template:Navbox with columns Template:Trans-Neptunian objects