2004 XR190
| Discovery | |
|---|---|
| Discovered by |
Lynne Jones Brett Gladman John J. Kavelaars Jean-Marc Petit Joel Parker Phil Nicholson |
| Discovery date | 11 December 2004 |
| Designations | |
| MPC designation | 2004 XR190 |
| none | |
|
cubewano detached object |
|
| Orbital characteristics | |
| Epoch 13 January 2016 (JD 2457400.5) | |
| Uncertainty parameter 3 | |
| Observation arc | 2957 days (8.10 yr) |
| Aphelion | 63.933 AU (9.5642 Tm) (Q) |
| Perihelion | 51.258 AU (7.6681 Tm) (q) |
| 57.595 AU (8.6161 Tm) (a) | |
| Eccentricity | 0.11003 (e) |
| 437.11 yr (159653 d) | |
| 277.502° (M) | |
| 0° 0m 8.118s /day (n) | |
| Inclination | 46.6656° (i) |
| 252.375042° (Ω) | |
| 282.724° (ω) | |
| Earth MOID | 50.557 AU (7.5632 Tm) |
| Jupiter MOID | 47.4512 AU (7.09860 Tm) |
| Physical characteristics | |
| Dimensions | 425–850 km (albedo 0.16–0.04) 335–530 km (albedo 0.25–0.10) |
| < 0.25? | |
| 22.04 | |
| 4.3 | |
2004 XR190 is a possible dwarf planet located in the scattered disc. It has a highly inclined low-eccentricity orbit. It was discovered in December 2004.
2004 XR190 was discovered on 11 December 2004. It was discovered by astronomers led by Lynne Jones of the University of British Columbia as part of the Canada–France Ecliptic Plane Survey (CFEPS) using the Canada–France–Hawaii Telescope (CFHT) near the ecliptic. In 2015, six precovery images from 2002 and 2003 were found in Sloan Digital Sky Survey data.
The discovery team nicknamed 2004 XR190 "Buffy", after the fictional vampire slayer, and proposed several Inuit-based official names to the IAU.
Considered a detached object,2004 XR190 is particularly unusual for two reasons. With an inclination of 47 degrees, it is the largest possible dwarf planet that has an inclination larger than 45 degrees, traveling further "up and down" than "left to right" around the Sun when viewed edge-on along the ecliptic. Second, it has an unusually circular orbit for a scattered-disc object (SDO). Although it is thought that traditional scattered-disc objects have been ejected into their current orbits by gravitational interactions with Neptune, the low eccentricity of its orbit and the distance of its perihelion (SDOs generally have highly eccentric orbits and perihelia less than 38 AU) seems hard to reconcile with such celestial mechanics. This has led to some uncertainty as to the current theoretical understanding of the outer Solar System. The theories include close stellar passages, rogue planets/planetary embryos in the early Kuiper belt, and resonance interaction with an outward-migrating Neptune. The Kozai mechanism is capable of transferring orbital eccentricity to a higher inclination.
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