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, 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]
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 and, 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 (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 is in an 8:3 resonance.[26] The likely dwarf planet 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 which are called extreme trans-Neptunian object (ETNOs)[28] may be trapped in the 5:3 and 3:1 mean-motion resonances with a putative Planet Nine with a semimajor axis ~700 AU.[29]
See also: Sednoid and Extreme trans-Neptunian object.
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.[30] [31] [32] [33] [34] [35]
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):[36]
| data-sort-type="number" width=130 | Designation | data-sort-type="number" | Diameter (km) | data-sort-type="number" | H | data-sort-type="number" | q (AU) | data-sort-type="number" | a (AU) | data-sort-type="number" | Q (AU) | data-sort-type="number" | ω (°) | data-sort-type="number" | Discovery Year | Discoverer | Notes & Refs |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| data-sort-value="148209" | 243 | 6.3 | 44.252 | 221.2 | 398 | 316.93 | 2000 | M. W. Buie | [37] | ||||||||
| data-sort-value="082075" | 216 | 4.7 | 41.207 | 57.795 | 74.383 | 316.481 | 2000 | Spacewatch | ≈3:8 Neptune resonance | ||||||||
| 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 | |||||||||
| data-sort-value="P2001K077A" | 634 | 5.0 | 43.41 | 47.74 | 52.07 | 120.3 | 2001 | M. W. Buie | borderline classical KBO | ||||||||
| data-sort-value="P2002C154P" | 222 | 6.5 | 42 | 52 | 62 | 50 | 2002 | M. W. Buie | orbit fairly poor, but definitely a detached object | ||||||||
| data-sort-value="P2003U291Y" | 147 | 7.4 | 41.19 | 48.95 | 56.72 | 15.6 | 2003 | M. W. Buie | borderline classical KBO | ||||||||
| data-sort-value="090377" | Sedna | 995 | 1.5 | 76.072 | 483.3 | 890 | 311.61 | 2003 | M. E. Brown, C. A. Trujillo, D. L. Rabinowitz | Sednoid | |||||||
| data-sort-value="P2004P112D" | 267 | 6.1 | 40 | 70 | 90 | 40 | 2004 | M. W. Buie | orbit very poor, might not be a detached object | ||||||||
| data-sort-value="474640" | Alicanto | 222 | 6.5 | 47.308 | 315 | 584 | 326.925 | 2004 | Cerro Tololo (unspecified) | [38] [39] [40] | |||||||
| data-sort-value="P2004X190R" | 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[41] [42] | ||||||||
| data-sort-value="P2005C081G" | 267 | 6.1 | 41.03 | 54.10 | 67.18 | 57.12 | 2005 | CFEPS | — | ||||||||
| data-sort-value="385607" | 161 | 7.2 | 41.215 | 62.98 | 84.75 | 349.86 | 2005 | M. W. Buie | — | ||||||||
| data-sort-value="145480" | 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 | ||||||||
| data-sort-value="P2006A101O" | 168 | 7.1 | — | — | — | — | 2006 | Mauna Kea (unspecified) | orbit extremely poor, might not be a TNO | ||||||||
| data-sort-value="278361" | 558 | 4.5 | 40.383 | 48.390 | 56.397 | 6.536 | 2007 | Palomar (unspecified) | borderline classical KBO | ||||||||
| data-sort-value="P2007L038E" | 176 | 7.0 | 41.798 | 54.56 | 67.32 | 53.96 | 2007 | Mauna Kea (unspecified) | — | ||||||||
| data-sort-value="P2008S291T" | 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 | ||||||||
| data-sort-value="P2009K036X" | 111 | 8.0 | — | 100 | 100 | — | 2009 | Mauna Kea (unspecified) | orbit extremely poor, might not be a TNO | ||||||||
| data-sort-value="P2010D093N" | 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 | ||||||||
| data-sort-value="P2010E065R" | 404 | 5.0 | 40.035 | 99.71 | 159.39 | 324.19 | 2010 | D. L. Rabinowitz, S. W. Tourtellotte | — | ||||||||
| data-sort-value="P2010G174B" | 222 | 6.5 | 48.8 | 360 | 670 | 347.7 | 2010 | Mauna Kea (unspecified) | — | ||||||||
| data-sort-value="P2012F084H" | 161 | 7.2 | 42 | 56 | 70 | 10 | 2012 | Las Campanas (unspecified) | — | ||||||||
| data-sort-value="P2012V113P" | 702 | 4.0 | 80.47 | 256 | 431 | 293.8 | 2012 | S. S. Sheppard, C. A. Trujillo | Sednoid | ||||||||
| data-sort-value="P2013Q028Q" | 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 | ||||||||
| data-sort-value="P2013F028T" | 202 | 6.7 | 43.5 | 310 | 580 | 40.3 | 2013 | S. S. Sheppard | — | ||||||||
| data-sort-value="496315" | 212 | 6.6 | 41.061 | 155.1 | 269.1 | 42.38 | 2013 | OSSOS | — | ||||||||
| data-sort-value="P2013G136Q" | 222 | 6.5 | 40.79 | 49.06 | 57.33 | 155.3 | 2013 | OSSOS | borderline classical KBO | ||||||||
| data-sort-value="P2013G138G" | 212 | 6.6 | 46.64 | 47.792 | 48.946 | 128 | 2013 | OSSOS | borderline classical KBO | ||||||||
| data-sort-value="500876" | 111 | 8.0 | 42.603 | 73.12 | 103.63 | 178.0 | 2013 | OSSOS | — | ||||||||
| data-sort-value="500880" | 147 | 7.4 | 44.04 | 48.158 | 52.272 | 179.8 | 2013 | OSSOS | borderline classical KBO | ||||||||
| data-sort-value="P2013S099Y" | 202 | 6.7 | 50.02 | 694 | 1338 | 32.1 | 2013 | OSSOS | — | ||||||||
| data-sort-value="P2013S100K" | 134 | 7.6 | 45.468 | 61.61 | 77.76 | 11.5 | 2013 | OSSOS | — | ||||||||
| data-sort-value="505478" | 255 | 6.3 | 43.89 | 195.7 | 348 | 252.33 | 2013 | OSSOS | — | ||||||||
| data-sort-value="P2013U017B" | 176 | 7.0 | 44.49 | 62.31 | 80.13 | 308.93 | 2013 | OSSOS | — | ||||||||
| data-sort-value="P2013V024D" | 128 | 7.8 | 40 | 50 | 70 | 197 | 2013 | Dark Energy Survey | orbit very poor, might not be a detached object | ||||||||
| data-sort-value="P2013Y151J" | 336 | 5.4 | 40.866 | 72.35 | 103.83 | 141.83 | 2013 | Pan-STARRS | — | ||||||||
| data-sort-value="P2014E051Z" | 770 | 3.7 | 40.70 | 52.49 | 64.28 | 329.84 | 2014 | Pan-STARRS | — | ||||||||
| data-sort-value="P2014F069C" | 533 | 4.6 | 40.28 | 73.06 | 105.8 | 190.57 | 2014 | S. S. Sheppard, C. A. Trujillo | |||||||||
| data-sort-value="P2014F071Z" | 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 | ||||||||
| data-sort-value="P2014F072C" | 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 | ||||||||
| data-sort-value="P2014J080M" | 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 | ||||||||
| data-sort-value="P2014J080S" | 306 | 5.5 | 40.013 | 48.291 | 56.569 | 174.5 | 2014 | Pan-STARRS | borderline classical KBO | ||||||||
| data-sort-value="P2014O394J" | 423 | 5.0 | 40.80 | 52.97 | 65.14 | 271.60 | 2014 | Pan-STARRS | in 3:7 Neptune resonance | ||||||||
| data-sort-value="P2014Q441R" | 193 | 6.8 | 42.6 | 67.8 | 93.0 | 283 | 2014 | Dark Energy Survey | — | ||||||||
| data-sort-value="P2014S349R" | 202 | 6.6 | 47.6 | 300 | 540 | 341.1 | 2014 | S. S. Sheppard, C. A. Trujillo | — | ||||||||
| data-sort-value="P2014S349S" | 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[43] | ||||||||
| data-sort-value="P2014S373T" | 330 | 5.5 | 50.13 | 104.0 | 157.8 | 297.52 | 2014 | Dark Energy Survey | — | ||||||||
| data-sort-value="P2014U228T" | 154 | 7.3 | 43.97 | 48.593 | 53.216 | 49.9 | 2014 | OSSOS | borderline classical KBO | ||||||||
| data-sort-value="P2014U230A" | 222 | 6.5 | 42.27 | 55.05 | 67.84 | 132.8 | 2014 | OSSOS | — | ||||||||
| data-sort-value="P2014U231O" | 97 | 8.3 | 42.25 | 55.11 | 67.98 | 234.56 | 2014 | OSSOS | — | ||||||||
| data-sort-value="P2014W509K" | 584 | 4.0 | 40.08 | 50.79 | 61.50 | 135.4 | 2014 | Pan-STARRS | — | ||||||||
| data-sort-value="P2014W556B" | 147 | 7.4 | 42.6 | 280 | 520 | 234 | 2014 | Dark Energy Survey | — | ||||||||
| data-sort-value="P2015A281L" | 293 | 6.1 | 42 | 48 | 54 | 120 | 2015 | Pan-STARRS | borderline classical KBO orbit very poor, might not be a detached object | ||||||||
| data-sort-value="495603" | 486 | 4.8 | 41.380 | 55.372 | 69.364 | 157.72 | 2015 | Pan-STARRS | — | ||||||||
| data-sort-value="487581" | 352 | 5.5 | 44.82 | 47.866 | 50.909 | 293.2 | 2015 | Pan-STARRS | borderline classical KBO | ||||||||
| data-sort-value="P2015F345J" | 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 | ||||||||
| data-sort-value="P2015G050P" | 222 | 6.5 | 40.4 | 55.2 | 70.0 | 130 | 2015 | S. S. Sheppard, C. A. Trujillo | — | ||||||||
| data-sort-value="P2015K162H" | 671 | 3.9 | 41.63 | 62.29 | 82.95 | 296.805 | 2015 | S. S. Sheppard, D. J. Tholen, C. A. Trujillo | — | ||||||||
| data-sort-value="P2015K163G" | 101 | 8.3 | 40.502 | 826 | 1610 | 32.06 | 2015 | OSSOS | — | ||||||||
| data-sort-value="P2015K163H" | 117 | 7.9 | 40.06 | 157.2 | 274 | 230.29 | 2015 | OSSOS | ≈1:12 Neptune resonance | ||||||||
| data-sort-value="P2015K172E" | 106 | 8.1 | 44.137 | 133.12 | 222.1 | 15.43 | 2015 | OSSOS | 1:9 Neptune resonance | ||||||||
| data-sort-value="P2015K172G" | 280 | 6.0 | 42 | 55 | 69 | 35 | 2015 | R. L. Allen D. James D. Herrera | orbit fairly poor, might not be a detached object | ||||||||
| data-sort-value="P2015K174Q" | 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 | ||||||||
| data-sort-value="P2015R245X" | 255 | 6.2 | 45.5 | 410 | 780 | 65.3 | 2015 | OSSOS | — | ||||||||
| data-sort-value="P2015T387G" | Leleākūhonua | 300 | 5.5 | 65.02 | 1042 | 2019 | 118.0 | 2015 | S. S. Sheppard, C. A. Trujillo, D. J. Tholen | Sednoid | |||||||
| 161 | 7.2 | 40.52 | 50.48 | 60.45 | 217.9 | 2017 | — | ||||||||||
| 168 | 7.1 | 40.88 | 47.99 | 55.1 | 218 | 2017 | borderline classical KBO | ||||||||||
| data-sort-value="P2017S132N" | 97 | 5.8 | 40.949 | 79.868 | 118.786 | 148.769 | 2017 | S. S. Sheppard, C. A. Trujillo, D. J. Tholen | |||||||||
| data-sort-value="P2018V035M" | 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.
| width=130 | Designation | data-sort-type="number" | Diameter (km) | data-sort-type="number" | H | data-sort-type="number" | q (AU) | data-sort-type="number" | a (AU) | data-sort-type="number" | Q (AU) | data-sort-type="number" | ω (°) | data-sort-type="number" | Discovery Year | Discoverer | Notes & Refs |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| data-sort-value="506479" | 147 | 7.4 | 38.116 | 166.2 | 294 | 11.082 | 2003 | Mauna Kea (unspecified) | — | ||||||||
| data-sort-value="P2003S422S" | 168 | data-slort-value="7.2" | 7.04 | 39.574 | 198.181 | 356.788 | 206.824 | 2003 | Cerro Tololo (unspecified) | — | |||||||
| data-sort-value="P2005R052H" | 128 | 7.8 | 38.957 | 152.6 | 266.3 | 32.285 | 2005 | CFEPS | — | ||||||||
| data-sort-value="P2007T434C" | 168 | 7.0 | 39.577 | 128.41 | 217.23 | 351.010 | 2007 | Las Campanas (unspecified) | 1:9 Neptune resonance | ||||||||
| data-sort-value="P2012F084L" | 212 | 6.6 | 38.607 | 106.25 | 173.89 | 141.866 | 2012 | Pan-STARRS | — | ||||||||
| data-sort-value="P2014F072L" | 193 | 6.8 | 38.1 | 104 | 170 | 259.49 | 2014 | Cerro Tololo (unspecified) | — | ||||||||
| data-sort-value="P2014J080W" | 352 | 5.5 | 38.161 | 142.62 | 247.1 | 131.61 | 2014 | Pan-STARRS | — | ||||||||
| data-sort-value="P2014Y050K" | 293 | 5.6 | 38.972 | 120.52 | 202.1 | 169.31 | 2014 | Pan-STARRS | — | ||||||||
| 8.78 | 39.491 | 272.302 | 505.113 | 43.227 | 2015 | OSSOS | |||||||||||
| data-sort-value="P2015G050T" | 88 | 8.6 | 38.46 | 333 | 627 | 129.3 | 2015 | OSSOS | — |