Plutino
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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, (208996) 2003 AZ84, and Ixion. Plutinos are named after mythological creatures associated with the underworld.
Plutinos form the inner part of the
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 semimajor axes close to the 3:2 Neptune resonance are primarily plutinos.[3]
Orbital characteristics
While the majority of plutinos have relatively low
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
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
Orbital diagrams
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The motions ofrotating 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-plutinoinclinationis 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.
Brightest objects
The plutinos brighter than HV=6 include:
| Object | a (AU) |
q (AU) |
i (°) |
H | Diameter (km) |
Mass (1020 kg) |
Albedo | V−R |
Discovery year |
Discoverer | Refs |
|---|---|---|---|---|---|---|---|---|---|---|---|
134340 Pluto |
39.3 | 29.7 | 17.1 | −0.7 | 2322 | 130 | 0.49–0.66 | 1930 | Clyde Tombaugh | JPL | |
| 90482 Orcus | 39.2 | 30.3 | 20.6 | 2.31±0.03 | 917±25 | 6.32±0.05 | 0.28±0.06 | 0.37 | 2004 | M. Brown, C. Trujillo, D. Rabinowitz |
JPL |
| (208996) 2003 AZ84 | 39.4 | 32.3 | 13.6 | 3.74±0.08 | 727.0+61.9 −66.5 |
≈ 3 | 0.107+0.023 −0.016 |
0.38±0.04 | 2003 | M. Brown, C. Trujillo |
JPL |
| 28978 Ixion | 39.7 | 30.1 | 19.6 | 3.828±0.039 | 617+19 −20 |
≈ 3 | 0.141±0.011 | 0.61 | 2001 | Deep Ecliptic Survey | JPL |
2017 OF69 |
39.5 | 31.3 | 13.6 | 4.091±0.12 | ≈ 380–680 | ? | ? | ? | 2017 | D. J. Tholen, S. S. Sheppard, C. Trujillo |
JPL |
| (84922) 2003 VS2 | 39.3 | 36.4 | 14.8 | 4.1±0.38 | 523.0+35.1 −34.4 |
≈ 1.5 | 0.147+0.063 −0.043 |
0.59±0.02 | 2003 | NEAT |
JPL |
| (455502) 2003 UZ413 | 39.2 | 30.4 | 12.0 | 4.38±0.05 | ≈ 600 | ≈ 2 | ? | 0.46±0.06 | 2001 | M. Brown, C. Trujillo, D. Rabinowitz |
JPL |
| 2014 JR80 | 39.5 | 36.0 | 15.4 | 4.9 | ≈ 240–670 | ? | ? | ? | 2014 | Pan-STARRS | JPL |
| 2014 JP80 | 39.5 | 36.7 | 19.4 | 4.9 | ≈ 240–670 | ? | ? | ? | 2014 | Pan-STARRS | JPL |
| 38628 Huya | 39.4 | 28.5 | 15.5 | 5.04±0.03 | 406±16 | ≈ 0.5 | 0.083±0.004 | 0.57±0.09 | 2000 | Ignacio Ferrin | JPL |
| (469987) 2006 HJ123 | 39.3 | 27.4 | 12.0 | 5.32±0.66 | 283.1+142.3 −110.8 |
≈ 0.012 | 0.136+0.308 −0.089 |
2006 | Marc W. Buie |
JPL | |
2002 XV93 |
39.3 | 34.5 | 13.3 | 5.42±0.46 | 549.2+21.7 −23.0 |
≈ 1.7 | 0.040+0.020 −0.015 |
0.37±0.02 | 2001 | M.W.Buie | JPL |
| (469372) 2001 QF298 | 39.3 | 34.9 | 22.4 | 5.43±0.07 | 408.2+40.2 −44.9 |
≈ 0.7 | 0.071+0.020 −0.014 |
0.39±0.06 | 2001 | Marc W. Buie | JPL |
| 47171 Lempo | 39.3 | 30.6 | 8.4 | 5.41±0.10 | 393.1+25.2 −26.8 (triple) |
0.1275±0.0006 | 0.079+0.013 −0.011 |
0.70±0.03 | 1999 | E. P. Rubenstein, L.-G. Strolger |
JPL |
| (307463) 2002 VU130 | 39.3 | 31.2 | 14.0 | 5.47±0.83 | 252.9+33.6 −31.3 |
≈ 0.16 | 0.179+0.202 −0.103 |
2002 | Marc W. Buie |
JPL | |
| (84719) 2002 VR128 | 39.3 | 28.9 | 14.0 | 5.58±0.37 | 448.5+42.1 −43.2 |
≈ 1 | 0.052+0.027 −0.018 |
0.60±0.02 | 2002 | NEAT | JPL |
| (55638) 2002 VE95 | 39.4 | 30.4 | 16.3 | 5.70±0.06 | 249.8+13.5 −13.1 |
≈ 0.15 | 0.149+0.019 −0.016 |
0.72±0.05 | 2002 | NEAT |
JPL |
(link to all of the orbits of these objects listed above are here)
See also
- Resonant Trans-Neptunian Object
- Twotino
References
- S2CID 10622344.
- S2CID 53772214. Retrieved 2019-07-20.
- ISBN 012446744X. Retrieved 2019-07-21.
- .
- .
- 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.
