Detached objects are a dynamical class of minor planets in the outer reaches of the Solar System and belong to the broader family of trans-Neptunian objects (TNOs). These objects have orbits whose points of closest approach to the Sun (perihelion) are sufficiently distant from the gravitational influence of Neptune that they are only moderately affected by Neptune and the other known planets: This makes them appear to be "detached" from the rest of the Solar System, except for their attraction to the Sun. [1] [2]
In this way, detached objects differ substantially from most other known TNOs, which form a loosely defined set of populations that have been perturbed to varying degrees onto their current orbit by gravitational encounters with the giant planets, predominantly Neptune. Detached objects have larger perihelia than these other TNO populations, including the objects in orbital resonance with Neptune, such as Pluto, the classical Kuiper belt objects in non-resonant orbits such as Makemake, and the scattered disk objects like Eris.
Detached objects have also been referred to in the scientific literature as extended scattered disc objects (E-SDO), [3] distant detached objects (DDO), [4] or scattered–extended, as in the formal classification by the Deep Ecliptic Survey. [5] This reflects the dynamical gradation that can exist between the orbital parameters of the scattered disk and the detached population.
At least nine such bodies have been securely identified, [6] of which the largest, most distant, and best known is Sedna. Those with large semi-major axes and high perihelion orbits similar to that of Sedna are termed sednoids. As of 2024, there are three known sednoids: Sedna, 2012 VP113, and Leleākūhonua. [7] These objects exhibit a highly statistically significant asymmetry between the distributions of object pairs with small ascending and descending nodal distances that might be indicative of a response to external perturbations; asymmetries such as this one are sometimes attributed to perturbations induced by unseen planets. [8] [9]
Detached objects have perihelia much larger than Neptune's aphelion. They often have highly elliptical, very large orbits with semi-major axes of up to a few hundred astronomical units (AU, the radius of Earth's orbit). Such orbits cannot have been created by gravitational scattering by the giant planets, not even Neptune. Instead, a number of explanations have been put forward, including an encounter with a passing star [10] or a distant planet-sized object, [4] or Neptune migration (which may once have had a much more eccentric orbit, from which it could have tugged the objects to their current orbit) [11] [12] [13] [14] [15] or ejected rogue planets (present in the early Solar System that were ejected). [16] [17] [18]
The classification suggested by the Deep Ecliptic Survey team introduces a formal distinction between scattered-near objects (which could be scattered by Neptune) and scattered-extended objects (e.g. 90377 Sedna) using a Tisserand's parameter value of 3. [5]
The Planet Nine hypothesis suggests that the orbits of several detached objects can be explained by the gravitational influence of a large, unobserved planet between 200 AU and 1200 AU from the Sun and/or the influence of Neptune. [19]
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Detached objects are one of four distinct dynamical classes of TNO; the other three classes are classical Kuiper-belt objects, resonant objects, and scattered-disc objects (SDO). [20] Sednoids also belong to detached objects. Detached objects generally have a perihelion distance greater than 40 AU, deterring strong interactions with Neptune, which has an approximately circular orbit about 30 AU from the Sun. The boundary between the scattered and detached regions can be defined using an analytical resonance overlap criterion. [21] [22]
The discovery of 90377 Sedna in 2003, together with a few other objects discovered around that time such as (148209) 2000 CR105 and (612911) 2004 XR190 , has motivated discussion of a category of distant objects that may also be inner Oort cloud objects or (more likely) transitional objects between the scattered disc and the inner Oort cloud. [2]
Although Sedna is officially considered a scattered-disc object by the MPC, its discoverer Michael E. Brown has suggested that because its perihelion distance of 76 AU is too distant to be affected by the gravitational attraction of the outer planets it should be considered an inner-Oort-cloud object rather than a member of the scattered disc. [23] This classification of Sedna as a detached object is accepted in recent publications. [24]
This line of thinking suggests that the lack of a significant gravitational interaction with the outer planets creates an extended–outer group starting somewhere between Sedna (perihelion 76 AU) and more conventional SDOs like 1996 TL66 (perihelion 35 AU), which is listed as a scattered–near object by the Deep Ecliptic Survey. [25]
One of the problems with defining this extended category is that weak resonances may exist and would be difficult to prove due to chaotic planetary perturbations and the current lack of knowledge of the orbits of these distant objects. They have orbital periods of more than 300 years and most have only been observed over a short observation arc of a couple years. Due to their great distance and slow movement against background stars, it may be decades before most of these distant orbits are determined well enough to confidently confirm or rule out a resonance. Further improvement in the orbit and potential resonance of these objects will help to understand the migration of the giant planets and the formation of the Solar System. For example, simulations by Emel'yanenko and Kiseleva in 2007 show that many distant objects could be in resonance with Neptune. They show a 10% likelihood that 2000 CR105 is in a 20:1 resonance, a 38% likelihood that 2003 QK91 is in a 10:3 resonance, and an 84% likelihood that (82075) 2000 YW134 is in an 8:3 resonance. [26] The likely dwarf planet (145480) 2005 TB190 appears to have less than a 1% likelihood of being in a 4:1 resonance. [26]
Mike Brown—who made the Planet Nine hypothesis—makes an observation that "all of the known distant objects which are pulled even a little bit away from the Kuiper seem to be clustered under the influence of this hypothetical planet (specifically, objects with semimajor axis > 100 AU and perihelion > 42 AU)". [27] Carlos de la Fuente Marcos and Ralph de la Fuente Marcos have calculated that some of the statistically significant commensurabilities are compatible with the Planet Nine hypothesis; in particular, a number of objects [a] which are called extreme trans-Neptunian object (ETNOs) [29] may be trapped in the 5:3 and 3:1 mean-motion resonances with a putative Planet Nine with a semimajor axis ~700 AU. [30]
This section needs to be updated. Please help update this section to reflect recent events or newly available information. Relevant discussion may be found on the talk page. (October 2023) |
This is a list of known objects by discovery date that could not be easily scattered by Neptune's current orbit and therefore are likely to be detached objects, but that lie inside the perihelion gap of ≈50–75 AU that defines the sednoids. [31] [32] [33] [34] [35] [36]
Objects listed below have a perihelion of more than 40 AU, and a semi-major axis of more than 47.7 AU (the 1:2 resonance with Neptune, and the approximate outer limit of the Kuiper Belt): [37]
Designation | Diameter [38] (km) | H | q (AU) | a (AU) | Q (AU) | ω (°) | Discovery Year | Discoverer | Notes & Refs |
---|---|---|---|---|---|---|---|---|---|
2000 CR105 | 243 | 6.3 | 44.252 | 221.2 | 398 | 316.93 | 2000 | M. W. Buie | [39] |
2000 YW134 | 216 | 4.7 | 41.207 | 57.795 | 74.383 | 316.481 | 2000 | Spacewatch | ≈3:8 Neptune resonance |
2001 FL193 | 81 | 8.7 | 40.29 | 50.26 | 60.23 | 108.6 | 2001 | R. L. Allen, G. Bernstein, R. Malhotra | orbit extremely poor, might not be a TNO |
2001 KA77 | 634 | 5.0 | 43.41 | 47.74 | 52.07 | 120.3 | 2001 | M. W. Buie | borderline classical KBO |
2002 CP154 | 222 | 6.5 | 42 | 52 | 62 | 50 | 2002 | M. W. Buie | orbit fairly poor, but definitely a detached object |
2003 UY291 | 147 | 7.4 | 41.19 | 48.95 | 56.72 | 15.6 | 2003 | M. W. Buie | borderline classical KBO |
Sedna | 995 | 1.5 | 76.072 | 483.3 | 890 | 311.61 | 2003 | M. E. Brown, C. A. Trujillo, D. L. Rabinowitz | Sednoid |
2004 PD112 | 267 | 6.1 | 40 | 70 | 90 | 40 | 2004 | M. W. Buie | orbit very poor, might not be a detached object |
Alicanto | 222 | 6.5 | 47.308 | 315 | 584 | 326.925 | 2004 | Cerro Tololo (unspecified) | [40] [41] [42] |
2004 XR190 | 612 | 4.1 | 51.085 | 57.336 | 63.586 | 284.93 | 2004 | R. L. Allen, B. J. Gladman, J. J. Kavelaars J.-M. Petit, J. W. Parker, P. Nicholson | very high inclination; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination of 2004 XR190 to obtain a very high perihelion [39] [43] [44] |
2005 CG81 | 267 | 6.1 | 41.03 | 54.10 | 67.18 | 57.12 | 2005 | CFEPS | — |
2005 EO297 | 161 | 7.2 | 41.215 | 62.98 | 84.75 | 349.86 | 2005 | M. W. Buie | — |
2005 TB190 | 372 | 4.5 | 46.197 | 75.546 | 104.896 | 171.023 | 2005 | A. C. Becker, A. W. Puckett, J. M. Kubica | Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion [44] |
2006 AO101 | 168 | 7.1 | — | — | — | — | 2006 | Mauna Kea (unspecified) | orbit extremely poor, might not be a TNO |
2007 JJ43 | 558 | 4.5 | 40.383 | 48.390 | 56.397 | 6.536 | 2007 | Palomar (unspecified) | borderline classical KBO |
2007 LE38 | 176 | 7.0 | 41.798 | 54.56 | 67.32 | 53.96 | 2007 | Mauna Kea (unspecified) | — |
2008 ST291 | 640 | 4.2 | 42.27 | 99.3 | 156.4 | 324.37 | 2008 | M. E. Schwamb, M. E. Brown, D. L. Rabinowitz | ≈1:6 Neptune resonance |
2009 KX36 | 111 | 8.0 | — | 100 | 100 | — | 2009 | Mauna Kea (unspecified) | orbit extremely poor, might not be a TNO |
2010 DN93 | 486 | 4.7 | 45.102 | 55.501 | 65.90 | 33.01 | 2010 | Pan-STARRS | ≈2:5 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion [44] |
2010 ER65 | 404 | 5.0 | 40.035 | 99.71 | 159.39 | 324.19 | 2010 | D. L. Rabinowitz, S. W. Tourtellotte | — |
2010 GB174 | 222 | 6.5 | 48.8 | 360 | 670 | 347.7 | 2010 | Mauna Kea (unspecified) | — |
2012 FH84 | 161 | 7.2 | 42 | 56 | 70 | 10 | 2012 | Las Campanas (unspecified) | — |
2012 VP113 | 702 | 4.0 | 80.47 | 256 | 431 | 293.8 | 2012 | S. S. Sheppard, C. A. Trujillo | Sednoid |
2013 FQ28 | 280 | 6.0 | 45.9 | 63.1 | 80.3 | 230 | 2013 | S. S. Sheppard, C. A. Trujillo | ≈1:3 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion [44] |
2013 FT28 | 202 | 6.7 | 43.5 | 310 | 580 | 40.3 | 2013 | S. S. Sheppard | — |
2013 GP136 | 212 | 6.6 | 41.061 | 155.1 | 269.1 | 42.38 | 2013 | OSSOS | — |
2013 GQ136 | 222 | 6.5 | 40.79 | 49.06 | 57.33 | 155.3 | 2013 | OSSOS | borderline classical KBO |
2013 GG138 | 212 | 6.6 | 46.64 | 47.792 | 48.946 | 128 | 2013 | OSSOS | borderline classical KBO |
2013 JD64 | 111 | 8.0 | 42.603 | 73.12 | 103.63 | 178.0 | 2013 | OSSOS | — |
2013 JJ64 | 147 | 7.4 | 44.04 | 48.158 | 52.272 | 179.8 | 2013 | OSSOS | borderline classical KBO |
2013 SY99 | 202 | 6.7 | 50.02 | 694 | 1338 | 32.1 | 2013 | OSSOS | — |
2013 SK100 | 134 | 7.6 | 45.468 | 61.61 | 77.76 | 11.5 | 2013 | OSSOS | — |
2013 UT15 | 255 | 6.3 | 43.89 | 195.7 | 348 | 252.33 | 2013 | OSSOS | — |
2013 UB17 | 176 | 7.0 | 44.49 | 62.31 | 80.13 | 308.93 | 2013 | OSSOS | — |
2013 VD24 | 128 | 7.8 | 40 | 50 | 70 | 197 | 2013 | Dark Energy Survey | orbit very poor, might not be a detached object |
2013 YJ151 | 336 | 5.4 | 40.866 | 72.35 | 103.83 | 141.83 | 2013 | Pan-STARRS | — |
2014 EZ51 | 770 | 3.7 | 40.70 | 52.49 | 64.28 | 329.84 | 2014 | Pan-STARRS | — |
2014 FC69 | 533 | 4.6 | 40.28 | 73.06 | 105.8 | 190.57 | 2014 | S. S. Sheppard, C. A. Trujillo | |
2014 FZ71 | 185 | 6.9 | 55.9 | 76.2 | 96.5 | 245 | 2014 | S. S. Sheppard, C. A. Trujillo | ≈1:4 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion [44] |
2014 FC72 | 509 | 4.5 | 51.670 | 76.329 | 100.99 | 32.85 | 2014 | Pan-STARRS | ≈1:4 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion [44] |
2014 JM80 | 352 | 5.5 | 46.00 | 63.00 | 80.01 | 96.1 | 2014 | Pan-STARRS | ≈1:3 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion [44] |
2014 JS80 | 306 | 5.5 | 40.013 | 48.291 | 56.569 | 174.5 | 2014 | Pan-STARRS | borderline classical KBO |
2014 OJ394 | 423 | 5.0 | 40.80 | 52.97 | 65.14 | 271.60 | 2014 | Pan-STARRS | in 3:7 Neptune resonance |
2014 QR441 | 193 | 6.8 | 42.6 | 67.8 | 93.0 | 283 | 2014 | Dark Energy Survey | — |
2014 SR349 | 202 | 6.6 | 47.6 | 300 | 540 | 341.1 | 2014 | S. S. Sheppard, C. A. Trujillo | — |
2014 SS349 | 134 | 7.6 | 45 | 140 | 240 | 148 | 2014 | S. S. Sheppard, C. A. Trujillo | ≈2:10 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a high perihelion [45] |
2014 ST373 | 330 | 5.5 | 50.13 | 104.0 | 157.8 | 297.52 | 2014 | Dark Energy Survey | — |
2014 UT228 | 154 | 7.3 | 43.97 | 48.593 | 53.216 | 49.9 | 2014 | OSSOS | borderline classical KBO |
2014 UA230 | 222 | 6.5 | 42.27 | 55.05 | 67.84 | 132.8 | 2014 | OSSOS | — |
2014 UO231 | 97 | 8.3 | 42.25 | 55.11 | 67.98 | 234.56 | 2014 | OSSOS | — |
2014 WK509 | 584 | 4.0 | 40.08 | 50.79 | 61.50 | 135.4 | 2014 | Pan-STARRS | — |
2014 WB556 | 147 | 7.4 | 42.6 | 280 | 520 | 234 | 2014 | Dark Energy Survey | — |
2015 AL281 | 293 | 6.1 | 42 | 48 | 54 | 120 | 2015 | Pan-STARRS | borderline classical KBO orbit very poor, might not be a detached object |
2015 AM281 | 486 | 4.8 | 41.380 | 55.372 | 69.364 | 157.72 | 2015 | Pan-STARRS | — |
2015 BE519 | 352 | 5.5 | 44.82 | 47.866 | 50.909 | 293.2 | 2015 | Pan-STARRS | borderline classical KBO |
2015 FJ345 | 117 | 7.9 | 51 | 63.0 | 75.2 | 78 | 2015 | S. S. Sheppard, C. A. Trujillo | ≈1:3 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion [44] |
2015 GP50 | 222 | 6.5 | 40.4 | 55.2 | 70.0 | 130 | 2015 | S. S. Sheppard, C. A. Trujillo | — |
2015 KH162 | 671 | 3.9 | 41.63 | 62.29 | 82.95 | 296.805 | 2015 | S. S. Sheppard, D. J. Tholen, C. A. Trujillo | — |
2015 KG163 | 101 | 8.3 | 40.502 | 826 | 1610 | 32.06 | 2015 | OSSOS | — |
2015 KH163 | 117 | 7.9 | 40.06 | 157.2 | 274 | 230.29 | 2015 | OSSOS | ≈1:12 Neptune resonance |
2015 KE172 | 106 | 8.1 | 44.137 | 133.12 | 222.1 | 15.43 | 2015 | OSSOS | 1:9 Neptune resonance |
2015 KG172 | 280 | 6.0 | 42 | 55 | 69 | 35 | 2015 | R. L. Allen D. James D. Herrera | orbit fairly poor, might not be a detached object |
2015 KQ174 | 154 | 7.3 | 49.31 | 55.40 | 61.48 | 294.0 | 2015 | Mauna Kea (unspecified) | ≈2:5 Neptune resonance; Neptune Mean Motion Resonance (MMR) along with the Kozai Resonance (KR) modified the eccentricity and inclination to obtain a very high perihelion [44] |
2015 RX245 | 255 | 6.2 | 45.5 | 410 | 780 | 65.3 | 2015 | OSSOS | — |
Leleākūhonua | 300 | 5.5 | 65.02 | 1042 | 2019 | 118.0 | 2015 | S. S. Sheppard, C. A. Trujillo, D. J. Tholen | Sednoid |
2017 DP121 | 161 | 7.2 | 40.52 | 50.48 | 60.45 | 217.9 | 2017 | — | |
2017 FP161 | 168 | 7.1 | 40.88 | 47.99 | 55.1 | 218 | 2017 | borderline classical KBO | |
2017 SN132 | 97 | 5.8 | 40.949 | 79.868 | 118.786 | 148.769 | 2017 | S. S. Sheppard, C. A. Trujillo, D. J. Tholen | |
2018 VM35 | 134 | 7.6 | 45.289 | 240.575 | 435.861 | 302.008 | 2018 | Mauna Kea (unspecified) |
The following objects can also be generally thought to be detached objects, although with slightly lower perihelion distances of 38–40 AU.
Designation | Diameter [38] (km) | H | q (AU) | a (AU) | Q (AU) | ω (°) | Discovery Year | Discoverer | Notes & Refs |
---|---|---|---|---|---|---|---|---|---|
2003 HB57 | 147 | 7.4 | 38.116 | 166.2 | 294 | 11.082 | 2003 | Mauna Kea (unspecified) | — |
2003 SS422 | 168 | 7.04 | 39.574 | 198.181 | 356.788 | 206.824 | 2003 | Cerro Tololo (unspecified) | — |
2005 RH52 | 128 | 7.8 | 38.957 | 152.6 | 266.3 | 32.285 | 2005 | CFEPS | — |
2007 TC434 | 168 | 7.0 | 39.577 | 128.41 | 217.23 | 351.010 | 2007 | Las Campanas (unspecified) | 1:9 Neptune resonance |
2012 FL84 | 212 | 6.6 | 38.607 | 106.25 | 173.89 | 141.866 | 2012 | Pan-STARRS | — |
2014 FL72 | 193 | 6.8 | 38.1 | 104 | 170 | 259.49 | 2014 | Cerro Tololo (unspecified) | — |
2014 JW80 | 352 | 5.5 | 38.161 | 142.62 | 247.1 | 131.61 | 2014 | Pan-STARRS | — |
2014 YK50 | 293 | 5.6 | 38.972 | 120.52 | 202.1 | 169.31 | 2014 | Pan-STARRS | — |
2015 DM319 | 8.78 | 39.491 | 272.302 | 505.113 | 43.227 | 2015 | OSSOS | ||
2015 GT50 | 88 | 8.6 | 38.46 | 333 | 627 | 129.3 | 2015 | OSSOS | — |
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.
A trans-Neptunian object (TNO), also written transneptunian object, is any minor planet in the Solar System that orbits the Sun at a greater average distance than Neptune, which has an orbital semi-major axis of 30.1 astronomical units (AU).
The scattered disc (or scattered disk) is a distant circumstellar disc in the Solar System that is sparsely populated by icy small Solar System bodies, which are a subset of the broader family of trans-Neptunian objects. The scattered-disc objects (SDOs) have orbital eccentricities ranging as high as 0.8, inclinations as high as 40°, and perihelia greater than 30 astronomical units (4.5×109 km; 2.8×109 mi). These extreme orbits are thought to be the result of gravitational "scattering" by the gas giants, and the objects continue to be subject to perturbation by the planet Neptune.
(612911) 2004 XR190, informally nicknamed Buffy, is a trans-Neptunian object, classified as both a scattered disc object and a detached object, located in the outermost region of the Solar System. It was first observed on 11 December 2004, by astronomers with the Canada–France Ecliptic Plane Survey at the Mauna Kea Observatories, Hawaii, United States. It is the largest known highly inclined (> 45°) object. With a perihelion of 51 AU, it belongs to a small and poorly understood group of very distant objects with moderate eccentricities.
(612584) 2003 QX113 is a large trans-Neptunian object from the scattered disc located in the outermost region of the Solar System. It is one of the most distant objects from the Sun at 60.5 AU. It was discovered by astronomers with the Canada–France Ecliptic Plane Survey at Mauna Kea Observatories, Hawaii, when it was near aphelion on 31 August 2003. It was provisionally designated 2003 QX113.
2012 VP113, also known by its nickname "Biden", is a trans-Neptunian object of the sednoid population, located in the outermost reaches of the Solar System. It was first observed on 5 November 2012 by American astronomers Scott Sheppard and Chad Trujillo at the Cerro Tololo Inter-American Observatory in Chile. The discovery was announced on 26 March 2014. The object probably measures somewhere between 300 and 1000 km in diameter, possibly large enough to be a dwarf planet.
A sednoid is a trans-Neptunian object with a large semi-major axis and a high perihelion, similar to the orbit of the dwarf planet Sedna. The consensus among astronomers is that there are only three objects that are known from this population: Sedna, 2012 VP113, and 541132 Leleākūhonua (2015 TG387). All three have perihelia greater than 60 AU. These objects lie outside an apparently nearly empty gap in the Solar System and have no significant interaction with the planets. They are usually grouped with the detached objects. Some astronomers consider the sednoids to be Inner Oort Cloud (IOC) objects, though the inner Oort cloud, or Hills cloud, was originally predicted to lie beyond 2,000 AU, beyond the aphelia of the three known sednoids.
An extreme trans-Neptunian object (ETNO) is a trans-Neptunian object orbiting the Sun well beyond Neptune (30 AU) in the outermost region of the Solar System. An ETNO has a large semi-major axis of at least 150–250 AU. The orbits of ETNOs are much less affected by the known giant planets than all other known trans-Neptunian objects. They may, however, be influenced by gravitational interactions with a hypothetical Planet Nine, shepherding these objects into similar types of orbits. The known ETNOs exhibit a highly statistically significant asymmetry between the distributions of object pairs with small ascending and descending nodal distances that might be indicative of a response to external perturbations.
Planet Nine is a hypothetical ninth planet in the outer region of the Solar System. Its gravitational effects could explain the peculiar clustering of orbits for a group of extreme trans-Neptunian objects (ETNOs), bodies beyond Neptune that orbit the Sun at distances averaging more than 250 times that of the Earth i.e. over 250 astronomical units (AU). These ETNOs tend to make their closest approaches to the Sun in one sector, and their orbits are similarly tilted. These alignments suggest that an undiscovered planet may be shepherding the orbits of the most distant known Solar System objects. Nonetheless, some astronomers question this conclusion and instead assert that the clustering of the ETNOs' orbits is due to observational biases, resulting from the difficulty of discovering and tracking these objects during much of the year.
(533560) 2014 JM80 (provisional designation 2014 JM80) is a trans-Neptunian object (TNO) from the scattered disc in the outermost Solar System, approximately 340 kilometers (210 miles) in diameter. It was discovered on 9 May 2010 by astronomers with the Pan-STARRS-1 survey at the Haleakala Observatory, Hawaii, in the United States. According to American astronomer Michael Brown, it is "possibly" a dwarf planet.
2014 FZ71 is a trans-Neptunian object, a scattered disc classified as a scattered and detached object, located in the outermost region of the Solar System. It was first observed on 24 March 2014, by a team led by American astronomer Scott Sheppard at the Cerro Tololo Inter-American Observatory in Chile. With its perihelion of almost 56 AU, it belongs to a small and poorly understood group of very distant objects with moderate eccentricities. The object is not a dwarf planet candidate as it only measures approximately 150 kilometers (93 miles) in diameter.
(690420) 2014 FC72 is a trans-Neptunian object, classified as a scattered and detached object, located in the outermost region of the Solar System. It was first observed on 24 March 2014 by astronomers with the Pan-STARRS survey at Haleakala Observatory, Hawaii, United States. With its perihelion distant from Neptune, it belongs to a small and poorly understood group of objects with moderate eccentricities. It is estimated to measure 500 kilometers (300 miles) in diameter, assuming a low albedo.
2015 FJ345 is a trans-Neptunian object and detached object, located in the scattered disc, the outermost region of the Solar System. It was first observed on 17 March 2015, by a team led by American astronomer Scott Sheppard at the Mauna Kea Observatories, in Hawaii, United States. With its perihelion of almost 51 AU, it belongs to a small and poorly understood group of very distant objects with moderate eccentricities. The object is not a dwarf planet candidate as it only measures approximately 120 kilometers (75 miles) in diameter.
2015 KQ174 is a trans-Neptunian object, both considered a scattered and detached object, located in the outermost region of the Solar System. The object with a moderately inclined and eccentric orbit measures approximately 154 kilometers (96 miles) in diameter. It was first observed on 24 May 2015, by astronomers at the Mauna Kea Observatories in Hawaii, United States.
(523635) 2010 DN93 (provisional designation 2010 DN93) is a trans-Neptunian object from in the scattered disc located in the outermost region of the Solar System. It was discovered on 26 February 2010, by astronomers with the Pan-STARRS survey at Haleakala Observatory on the island of Maui, Hawaii, in the United States. Assuming a low albedo, the object is estimated at approximately 490 kilometers (300 miles) in diameter. It was numbered in 2018 and remains unnamed.
2013 FQ28 is a trans-Neptunian object, both considered a scattered and detached object, located in the outermost region of the Solar System. It was first observed on 17 March 2013, by a team of astronomers at the Cerro Tololo Inter-American Observatory in Chile. It orbits the Sun in a moderate inclined, moderate-eccentricity orbit. The weak dwarf planet candidate measures approximately 260 kilometers (160 miles) in diameter.
The hypothetical Planet Nine would modify the orbits of extreme trans-Neptunian objects via a combination of effects. On very long timescales exchanges of angular momentum with Planet Nine cause the perihelia of anti-aligned objects to rise until their precession reverses direction, maintaining their anti-alignment, and later fall, returning them to their original orbits. On shorter timescales mean-motion resonances with Planet Nine provides phase protection, which stabilizes their orbits by slightly altering the objects' semi-major axes, keeping their orbits synchronized with Planet Nine's and preventing close approaches. The inclination of Planet Nine's orbit weakens this protection, resulting in a chaotic variation of semi-major axes as objects hop between resonances. The orbital poles of the objects circle that of the Solar System's Laplace plane, which at large semi-major axes is warped toward the plane of Planet Nine's orbit, causing their poles to be clustered toward one side.
2014 ST373 (prov. designation:2014 ST373) is a trans-Neptunian object and a detached object from the outermost region of the Solar System. With a perihelion of 50.2 AU, it belongs to the top 10 minor planets with the highest known perihelia of the Solar System. and is neither a scattered disc nor an extreme trans-Neptunian object. It measures approximately 370 kilometers (230 miles) in diameter and was first observed on 25 September 2014, by astronomers using the Dark Energy Camera (DECam) at Cerro Tololo Inter-American Observatory in Chile.
Diameter: 242km
Discoverer: CTIO