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Plutino - Wikipedia

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In astronomy, a dynamical group of trans-Neptunian objects

This article is about the dynamical group and is not to be confused with

or

.

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 Orcus, Achlys, and Ixion. 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.

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]

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:

• 2005 TV₁₈₉, which follows the most highly inclined orbit (34.5°)
• (15875) 1996 TP66, which has the most elliptical orbit (its eccentricity is 0.33), with the perihelion halfway between Uranus and Neptune
• (470308) 2007 JH43 following a quasi-circular orbit
• 2002 VX₁₃₀ 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.

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 Ga timescales.^[6]

• 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.

• Orbits and sizes of the larger plutinos (and the reference non-plutino

  2002 KX₁₄

  ). 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

  2002 KX₁₄

  ). Small inserts show

  histograms

  for the distributions of orbital inclination and eccentricity.

The plutinos brighter than H_V=6 include:

(link to all of the orbits of these objects listed above are here)

• Astronomy portal

• Resonant Trans-Neptunian Object
• Twotino

1. ^ Malhotra, Renu (1995). "The Origin of Pluto's Orbit: Implications for the Solar System Beyond Neptune". Astronomical Journal. 110: 420. arXiv:astro-ph/9504036. Bibcode:1995AJ....110..420M. doi:10.1086/117532. S2CID 10622344.
2. ^ Almeida, A.J.C; Peixinho, N.; Correia, A.C.M. (December 2009). "Neptune Trojans & Plutinos: Colors, sizes, dynamics, & their possible collisions". Astronomy & Astrophysics. 508 (2): 1021–1030. arXiv:0910.0865. doi:10.1051/0004-6361/200911943. S2CID 53772214. Retrieved 2019-07-20.
3. ^ Lewis, John S. (2004). Physics & Chemistry of the Solar System. Centaurs & Trans-Neptunian Objects. Academic Press. pp. 409–412. ISBN 012446744X. Retrieved 2019-07-21.
4. ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (2016). "The analemma criterion: accidental quasi-satellites are indeed true quasi-satellites". Monthly Notices of the Royal Astronomical Society. 462 (3): 3344–3349. arXiv:1607.06686. Bibcode:2016MNRAS.462.3344D. doi:10.1093/mnras/stw1833.
5. ^ Wan, X.-S; Huang, T.-Y. (2001). "The orbit evolution of 32 plutinos over 100 million year". Astronomy and Astrophysics. 368 (2): 700–705. Bibcode:2001A&A...368..700W. doi:10.1051/0004-6361:20010056.
6. ^ Yu, Qingjuan; Tremaine, Scott (1999). "The Dynamics of Plutinos". Astronomical Journal. 118 (4): 1873–1881. arXiv:astro-ph/9904424. Bibcode:1999AJ....118.1873Y. doi:10.1086/301045. S2CID 14482507.

• 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., ISBN 3-540-26056-0 (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.

• David Jewitt on Plutinos
• Minor Planet Center, List of TNOs
• MPC List of Distant Minor Planets

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