2004 XR190
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Discovery
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| Discovered by | Lynne Jones, Brett Gladman, John J. Kavelaars, Jean-Marc Petit, Joel Parker, Phil Nicholson |
| Discovery date | December 11, 2004 |
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Designations
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| MPC designation | 2004 XR190 |
| Alternate name(s) | none |
| Minor planet category |
detached object |
| Epoch 2455200.5 (2010-Jan-04.0) | |
| Aphelion | 63.54 AU (9506 Gm) |
| Perihelion | 51.41 AU (7691 Gm) |
| Semi-major axis | 57.48 AU (8599 Gm) |
| Eccentricity | 0.1055 |
| Orbital period | 435.78 a (159169 d) |
| Average orbital speed | 3.92 km/s |
| Mean anomaly | 271.198° |
| Inclination | 46.66° |
| Longitude of ascending node | 252.364° |
| Argument of perihelion | 283.530° |
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Physical characteristics
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| Dimensions | 425–850 km (albedo 0.16-0.04)[1] 335–530 km (albedo 0.25-0.10)[2] |
| Mass | 0.6–4.8×1020 kg |
| Albedo | <0.25? |
| Temperature | ~37–36 K |
| Apparent magnitude | 22.04[3] |
| Absolute magnitude (H) | 4.5 |
2004 XR190 (also written 2004 XR190) is a dwarf-planet candidate located in the scattered disc. Astronomers led by Lynne Jones of the University of British Columbia made the discovery as part of the Canada-France Ecliptic Plane Survey (CFEPS) using the Canada-France-Hawaii Telescope (CFHT). The discovery team has temporarily nicknamed the object "Buffy", after the fictional vampire slayer, and proposed a different official name to the IAU.
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[edit] Orbit
Considered a detached object,[4][5] 2004 XR190 is particularly unusual for two reasons. With an inclination of 47 degrees, it is the most "tilted" dwarf-planet candidate discovered thus far, 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). While 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 the orbital eccentricity into an elevated inclination.[1]
[edit] Eleventh-most-distant body
2004 XR190 came to aphelion around 1901.[6] Other than long-period comets and space probes[7], it is currently the eleventh-most-distant known large body (57.9 AU)[3] in the Solar System after Eris and Dysnomia (both 96.6 AU)[8], Sedna (87.2 AU)[9], 2007 OR10 (86.3 AU)[10], 2006 QH181 (82.4 AU)[11], 2006 AO101 (63.9 AU), 2004 UT10 (61.1 AU), 2007 TB418 (59.4 AU), 2003 QX113 (59.3 AU)[12], and 1999 DP8 (59.2 AU).[13]
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A side view of 2004 XR190's orbit, showing the object's high inclination. Units are AUs.
[edit] Size
The object has a diameter estimated at around 500 kilometres, roughly a quarter the size of Pluto, and orbits between 51 and 64 AU (7.7 and 9.5 billion km) from the Sun.
[edit] References
- ^ a b R. L. Allen, B. Gladman (2006). "Discovery of a low-eccentricity, high-inclination Kuiper Belt object at 58 AU". The Astrophysical Journal 640: L83. Bibcode 2006ApJ...640L..83A. doi:10.1086/503098. Discovery paper. Preprint
- ^ E. L. Schaller and M. E. Brown (2007). "Volatile loss and retention on Kuiper belt objects". Astrophysical Journal 659: I.61–I.64. Bibcode 2007ApJ...659L..61S. doi:10.1086/516709. http://www.gps.caltech.edu/~mbrown/papers/ps/volatiles.pdf. Retrieved 2008-04-02.
- ^ a b "AstDys 2004 XR190 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2004XR190. Retrieved 2011-05-16.
- ^ Jewitt, David, Morbidelli, Alessandro, & Rauer, Heike. (2007). Trans-Neptunian Objects and Comets: Saas-Fee Advanced Course 35. Swiss Society for Astrophysics and Astronomy. Berlin: Springer. ISBN 3-540-71957-1.
- ^ Lykawka, Patryk Sofia & Mukai, Tadashi. (2007). Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation. Icarus Volume 189, Issue 1, July , Pages 213-232. doi:10.1016/j.icarus.2007.01.001.
- ^ "Horizon Online Ephemeris System". California Institute of Technology, Jet Propulsion Laboratory. http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=2004XR190. Retrieved 2009-03-23.
- ^ Chris Peat. "Spacecraft escaping the Solar System". Heavens-Above. http://www.heavens-above.com/solar-escape.asp. Retrieved 2008-04-03.
- ^ "AstDys (136199) Eris Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=Eris. Retrieved 2011-05-05.
- ^ "AstDys (90377) Sedna Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=Sedna. Retrieved 2011-05-05.
- ^ "AstDys (225088) 2007 OR10 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2007%20OR10. Retrieved 2011-05-05.
- ^ "AstDys 2006 QH181 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2006%20QH181. Retrieved 2011-05-05.
- ^ "AstDys 2003 QX113 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2003QX113. Retrieved 2011-05-05.
- ^ "MPEC 2010-A05 Distant Minor Planets (2010 JAN. 14.0 TT)". IAU Minor Planet Center. http://www.cfa.harvard.edu/mpec/K10/K10A05.html. Retrieved 2010-01-02.
[edit] External links
- MPEC circular detailing discovery
- Discovery webpage by research team
- Maggie McKee (2005-12-13). "Strange new object found at edge of Solar System". New Scientist. http://www.newscientist.com/article.ns?id=dn8455&feedId=online-news_rss20.
- Canada-France-Hawaii Telescope Legacy Survey
- Orbital simulation from JPL (Java) / Ephemeris
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