Detached object
Adapted from Wikipedia · Discoverer experience
Detached objects are a special group of small planets found far away from the Sun, in a part of space called the outer Solar System. These objects belong to a larger family known as trans-Neptunian objects, which orbit beyond the planet Neptune. What makes detached objects different is their distance from the Sun. They orbit so far out that the gravity of Neptune and other planets barely affects them, making them seem "detached" from the rest of the Solar System.
Unlike most other trans-Neptunian objects, which have been moved by the gravity of large planets like Neptune, detached objects stay in orbits that are far away from these influences. They have points of closest approach to the Sun that are much larger than those of other objects, such as Pluto, Makemake, and Eris. Because of this, scientists sometimes call them extended scattered disc objects, distant detached objects, or scattered–extended objects.
Scientists have found at least nine of these detached objects. The most famous one is Sedna, which is the largest, farthest, and best known. Objects like Sedna, with very large orbits and very distant points of closest approach to the Sun, are called sednoids. As of 2025, four sednoids are known, including 2012 VP113, Leleākūhonua, and 2023 KQ14. These objects show patterns in their orbits that might be caused by the pull of planets we have not yet discovered.
Orbits
Detached objects have orbits that stay very far from the Sun. Their closest points to the Sun are much larger than the farthest point of Neptune's orbit. These objects often have very stretched-out, long paths around the Sun, reaching up to a few hundred times the distance from the Earth to the Sun.
Scientists are still trying to understand how these objects got their unusual orbits. Some ideas include the pull of a passing star, a very far-off object about the size of a planet, or the movement of Neptune long ago. Another idea is the possible influence of a large, unseen planet far beyond Neptune.
Classification
Detached objects are a special group of objects far from the Sun in our Solar System. They belong to a larger group called trans-Neptunian objects (TNOs). Unlike most TNOs, detached objects have orbits that keep them far away from the planet Neptune. This distance means Neptune's gravity does not affect them much, making them seem "detached" from the rest of the Solar System.
These objects usually come closer to the Sun (perihelion) at a distance greater than 40 AU, which is much farther than Neptune's orbit. Because of this, they do not interact strongly with Neptune. Some scientists think these objects might be part of a region called the inner Oort cloud or a link between a group of objects called the scattered disc and the Oort cloud. Studying these objects helps us learn more about how the giant planets moved and how the Solar System formed.
Possible detached objects
See also: Sednoid and Extreme trans-Neptunian object
This is a list of objects found by discovery date that might be detached objects because they are not easily moved by Neptune's orbit. They are close to the Sun but still far enough to seem "detached" from the rest of the Solar System.
These objects have points where they get closest to the Sun (perihelion) more than 40 AU away and their average distance from the Sun (semi-major axis) is more than 47.7 AU away.
Some other objects are also thought to be detached objects, though they are a little closer to the Sun, with perihelion distances between 38–40 AU.
| Designation | Diameter (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 | |
| 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) | |
| 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 |
| 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 |
| 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 |
| 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 |
| 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 |
| 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 |
| 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 |
| 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 |
| 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 |
| 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 |
| 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) |
| Designation | Diameter (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 | — |
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