Utente:IndyJr/TNO distaccati
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| Designation | Diameter (km) |
H | q (AU) |
a (AU) |
Q (AU) |
ω (°) | Discovery Year |
Discoverer | Notes & Refs |
|---|---|---|---|---|---|---|---|---|---|
| Template:Mpl- | 243 | 6.3 | 44.252 | 221.2 | 398 | 316.93 | 2000 | M. W. Buie | [1] |
| Template:Mpl- | 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 |
| Template:Mpl- | 222 | 6.5 | 47.308 | 315 | 584 | 326.925 | 2004 | Cerro Tololo (unspecified) | [2][3][4] |
| 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 |
pseudo-Sednoid, 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[5][6] |
| 2005 CG81 | 267 | 6.1 | 41.03 | 54.10 | 67.18 | 57.12 | 2005 | CFEPS | — |
| Template:Mpl- | 161 | 7.2 | 41.215 | 62.98 | 84.75 | 349.86 | 2005 | M. W. Buie | — |
| Template:Mpl- | 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 |
| Template:Mpl- | 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 |
| Template:Mpl- | 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 | — |
| Template:Mpl- | 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 |
| Template:Mpl- | 111 | 8.0 | 42.603 | 73.12 | 103.63 | 178.0 | 2013 | OSSOS | — |
| Template:Mpl- | 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 | — |
| Template:Mpl- | 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 | pseudo-Sednoid; ≈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 | pseudo-Sednoid; ≈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[7] |
| 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 |
| Template:Mpl- | 486 | 4.8 | 41.380 | 55.372 | 69.364 | 157.72 | 2015 | Pan-STARRS | — |
| Template:Mpl- | 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 | pseudo-Sednoid; ≈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) | pseudo-Sednoid; ≈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 | ??? |
I TNO distaccati sono una classe dinamica di pianeti minori nei confini esterni del sistema solare e appartengono alla più ampia famiglia di oggetti transnettuniani (TNO). Questi oggetti hanno orbite i cui punti più vicini al Sole (perielio) sono sufficientemente distanti dall'influenza gravitazionale di Nettuno da essere solo moderatamente influenzati da quest'ultimo e dagli altri pianeti conosciuti: questo li fa sembrare "staccati" dal resto del sistema solare, tranne che per il loro legame gravitazione con il Sole.[8][9]
I TNO distaccati differiscono sostanzialmente dalla maggior parte degli altri TNO noti, che formano un insieme vagamente definito di popolazioni che sono state perturbate a vari livelli sulla loro orbita attuale da incontri gravitazionali con i pianeti giganti, prevalentemente Nettuno. I TNO distaccati hanno perieli più grandi di queste altre popolazioni TNO, inclusi gli oggetti in risonanza orbitale con Nettuno, come Plutone, i classici oggetti della cintura di Kuiper in orbite non risonanti come Makemake e gli oggetti del disco diffuso come Eris.
I TNO distaccati sono stati indicati nella letteratura scientifica anche come oggetti del disco diffuso esteso (E-SDO),[10] oggetti distaccati distanti (DDO),[11] o estesi diffusi, come nella classificazione formale del Deep Ecliptic Survey.[12] Ciò riflette la gradazione dinamica che può esistere tra i parametri orbitali del disco diffuso e la popolazione distaccata.
Almeno nove di questi corpi sono stati identificati in modo sicuro[13] di cui il più grande, il più distante e il più noto è Sedna. Quelli con perielio maggiore di 50 au sono chiamati sednoidi. A partire dal 2018, ci sono tre sednoidi conosciuti, Sedna, 2012 VP113 e Leleākūhonua .
Orbite[modifica | modifica wikitesto]
I TNO distaccati hanno il perielio molto più grande dell'afelio di Nettuno. Spesso hanno orbite molto ellittiche e molto grandi con semiassi maggiori fino a poche centinaia di unità astronomiche (au, il raggio dell'orbita terrestre). Tali orbite non possono essere state determinate dalle perturbazioni gravitazionali dei pianeti giganti, nemmeno da Nettuno. Invece, sono state avanzate una serie di spiegazioni, incluso un incontro con una stella di passaggio[14] o un oggetto distante delle dimensioni di un pianeta, [11] o lo stesso Nettuno (che un tempo potrebbe aver avuto un'orbita molto più eccentrica, da cui potrebbe aver trascinato gli oggetti nella loro orbita attuale) [15] [16] [17] [18] [19] o espulso pianeti (presenti nel primo sistema solare che furono espulsi). [20] [21] [22]
Gli oggetti elencati di seguito hanno un perielio superiore a 40 AU e un semiasse maggiore di oltre 47,7 AU (la risonanza 1: 2 con Nettuno e il limite esterno approssimativo della fascia di Kuiper) [23]
| Designation | Diameter (km) |
H | q (AU) |
a (AU) |
Q (AU) |
ω (°) | Discovery Year |
Discoverer | Notes & Refs |
|---|---|---|---|---|---|---|---|---|---|
| Template:Mpl- | 243 | 6.3 | 44.252 | 221.2 | 398 | 316.93 | 2000 | M. W. Buie | [1] |
| Template:Mpl- | 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 |
| Template:Mpl- | 222 | 6.5 | 47.308 | 315 | 584 | 326.925 | 2004 | Cerro Tololo (unspecified) | [2][3][4] |
| 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 |
pseudo-Sednoid, 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[24][6] |
| 2005 CG81 | 267 | 6.1 | 41.03 | 54.10 | 67.18 | 57.12 | 2005 | CFEPS | — |
| Template:Mpl- | 161 | 7.2 | 41.215 | 62.98 | 84.75 | 349.86 | 2005 | M. W. Buie | — |
| Template:Mpl- | 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 |
| Template:Mpl- | 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 |
| Template:Mpl- | 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 | — |
| Template:Mpl- | 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 |
| Template:Mpl- | 111 | 8.0 | 42.603 | 73.12 | 103.63 | 178.0 | 2013 | OSSOS | — |
| Template:Mpl- | 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 | — |
| Template:Mpl- | 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 | pseudo-Sednoid; ≈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 | pseudo-Sednoid; ≈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[7] |
| 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 |
| Template:Mpl- | 486 | 4.8 | 41.380 | 55.372 | 69.364 | 157.72 | 2015 | Pan-STARRS | — |
| Template:Mpl- | 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 | pseudo-Sednoid; ≈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) | pseudo-Sednoid; ≈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 | ??? |
Note[modifica | modifica wikitesto]
- ^ a b E. L. Schaller e M. E. Brown, Volatile loss and retention on Kuiper belt objects (PDF), in Astrophysical Journal, vol. 659, n. 1, 2007, pp. I.61–I.64, Bibcode:2007ApJ...659L..61S, DOI:10.1086/516709. URL consultato il 2 aprile 2008.E. L. Schaller; M. E. Brown (2007). "Volatile loss and retention on Kuiper belt objects" (PDF). Astrophysical Journal. 659 (1): I.61–I.64. Bibcode:2007ApJ...659L..61S. doi:10.1086/516709. Retrieved 2008-04-02. Errore nelle note: Tag
<ref>non valido; il nome "abc" è stato definito più volte con contenuti diversi - ^ a b boulder.swri.edu, http://www.boulder.swri.edu/~buie/kbo/astrom/04VN112.html. URL consultato il 17 luglio 2008.Buie, Marc W. (8 November 2007). "Orbit Fit and Astrometric record for 04VN112". SwRI (Space Science Department). Archived from the original on 18 August 2010. Retrieved 17 July 2008. Errore nelle note: Tag
<ref>non valido; il nome "VN112" è stato definito più volte con contenuti diversi - ^ a b ssd.jpl.nasa.gov, http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2004VN112. URL consultato il 24 febbraio 2015."JPL Small-Body Database Browser: (2004 VN112)". Retrieved 2015-02-24. Errore nelle note: Tag
<ref>non valido; il nome "jpldata04VN112" è stato definito più volte con contenuti diversi - ^ a b minorplanetcenter.net, http://www.minorplanetcenter.net/iau/lists/Centaurs.html. URL consultato il 5 luglio 2011.«Discoverer: CTIO»"List Of Centaurs and Scattered-Disk Objects". Retrieved 5 July 2011.
Discoverer: CTIO
Errore nelle note: Tag<ref>non valido; il nome "cen_sdo" è stato definito più volte con contenuti diversi - ^ R. L. Allen e B. Gladman, Discovery of a low-eccentricity, high-inclination Kuiper Belt object at 58 AU, in The Astrophysical Journal, vol. 640, n. 1, 2006, pp. L83–L86, Bibcode:2006ApJ...640L..83A, DOI:10.1086/503098, arXiv:astro-ph/0512430.
- ^ a b Scott S. Sheppard, Chadwick Trujillo e David J. Tholen, Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects with Moderate Semimajor Axes and Eccentricities, in The Astrophysical Journal Letters, vol. 825, n. 1, July 2016, p. L13, Bibcode:2016ApJ...825L..13S, DOI:10.3847/2041-8205/825/1/L13, arXiv:1606.02294.Sheppard, Scott S.; Trujillo, Chadwick; Tholen, David J. (July 2016). "Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects with Moderate Semimajor Axes and Eccentricities". The Astrophysical Journal Letters. 825 (1): L13. arXiv:1606.02294. Bibcode:2016ApJ...825L..13S. doi:10.3847/2041-8205/825/1/L13. S2CID 118630570. Errore nelle note: Tag
<ref>non valido; il nome "Like Buffy" è stato definito più volte con contenuti diversi - ^ a b Scott S. Sheppard e Chad Trujillo, New Extreme Trans-Neptunian Objects: Towards a Super-Earth in the Outer Solar System, in Astrophysical Journal, vol. 152, n. 6, August 2016, pp. 221, Bibcode:2016AJ....152..221S, DOI:10.3847/1538-3881/152/6/221, arXiv:1608.08772.Sheppard, Scott S.; Trujillo, Chad (August 2016). "New Extreme Trans-Neptunian Objects: Towards a Super-Earth in the Outer Solar System". Astrophysical Journal. 152 (6): 221. arXiv:1608.08772. Bibcode:2016AJ....152..221S. doi:10.3847/1538-3881/152/6/221. S2CID 119187392. Errore nelle note: Tag
<ref>non valido; il nome "Like 2014SS349" è stato definito più volte con contenuti diversi - ^ Lykawka, P.S. e Mukai, T., An outer planet beyond Pluto and the origin of the trans-Neptunian belt architecture, in Astronomical Journal, vol. 135, n. 4, 2008, pp. 1161–1200, Bibcode:2008AJ....135.1161L, DOI:10.1088/0004-6256/135/4/1161, arXiv:0712.2198.
- ^ D. Jewitt e A. Delsanti, The Solar System Beyond the Planets (PDF), in Solar System Update: Topical and Timely Reviews in Solar System Sciences, Springer-Praxisª ed., 2006, ISBN 3-540-26056-0.
- ^ B. Gladman, Evidence for an extended scattered disk, in Icarus, vol. 157, n. 2, 2002, pp. 269–279, Bibcode:2002Icar..157..269G, DOI:10.1006/icar.2002.6860, arXiv:astro-ph/0103435.
- ^ a b Rodney S. Gomes, J. Matese e Jack Lissauer, A distant planetary-mass solar companion may have produced distant detached objects, in Icarus, vol. 184, n. 2, Elsevier, 2006, pp. 589–601, Bibcode:2006Icar..184..589G, DOI:10.1016/j.icarus.2006.05.026.
Errore nelle note: Tag
<ref>non valido; il nome "Gomez 2006" è stato definito più volte con contenuti diversi - ^ Elliot, J.L., Kern, S.D. e Clancy, K.B., The Deep Ecliptic Survey: A search for Kuiper belt objects and centaurs. II. Dynamical classification, the Kuiper belt plane, and the core population (PDF), in The Astronomical Journal, vol. 129, n. 2, 2006, pp. 1117–1162, Bibcode:2005AJ....129.1117E, DOI:10.1086/427395.
- ^ Lykawka, Patryk Sofia e Mukai, Tadashi, Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation, in Icarus, vol. 189, n. 1, July 2007, pp. 213–232, Bibcode:2007Icar..189..213L, DOI:10.1016/j.icarus.2007.01.001.
- ^ Alessandro Morbidelli e Harold F. Levison, Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects [[:Template:Mp]] and [[:Template:Mp]], in The Astronomical Journal, vol. 128, n. 5, November 2004, pp. 2564–2576, Bibcode:2004AJ....128.2564M, DOI:10.1086/424617, arXiv:astro-ph/0403358. Wikilink compreso nell'URL del titolo (aiuto)
- ^ B. Gladman, M. Holman e T. Grav, Evidence for an extended scattered disk, in Icarus, vol. 157, n. 2, 2002, pp. 269–279, Bibcode:2002Icar..157..269G, DOI:10.1006/icar.2002.6860, arXiv:astro-ph/0103435.
- ^ grantchronicles.com, http://www.grantchronicles.com/12thplanetmk.htm.
- ^ sciencenews.org, https://www.sciencenews.org/article/comets-odd-orbit-hints-hidden-planet?mode=magazine&context=293.
- ^ spaceref.com, http://www.spaceref.com/news/viewnews.html?id=309.
- ^ sciencemag.org, http://www.sciencemag.org/news/2001/03/signs-hidden-planet.
- ^ Phil Mozel, Dr. Brett Gladman, in Journal of the Royal Astronomical Society of Canada, A moment with ..., vol. 105, n. 2, 2011, pp. 77, Bibcode:2011JRASC.105...77M.
- ^ Brett Gladman e Collin Chan, Production of the Extended Scattered Disk by Rogue Planets, in The Astrophysical Journal, vol. 643, n. 2, 2006, pp. L135–L138, Bibcode:2006ApJ...643L.135G, DOI:10.1086/505214.
- ^ findplanetnine.com, http://www.findplanetnine.com/2016/01/the-long-and-winding-history-of-planet-x.html.
- ^ minorplanetcenter.net, http://minorplanetcenter.net/db_search/show_by_properties?perihelion_distance_min=40&semimajor_axis_min=47.7. URL consultato il 7 May 2018.
- ^ R. L. Allen e B. Gladman, Discovery of a low-eccentricity, high-inclination Kuiper Belt object at 58 AU, in The Astrophysical Journal, vol. 640, n. 1, 2006, pp. L83–L86, Bibcode:2006ApJ...640L..83A, DOI:10.1086/503098, arXiv:astro-ph/0512430.
[[Categoria:Oggetti del disco diffuso]]