(612911) 2004 XR190: Difference between revisions

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==Orbit==
==Orbit==
Considered a [[detached object]],<ref name="Swiss">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.<!-- Page 86. --></ref><ref name="LykDyn">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}}.</ref> {{mp|2004 XR|190}} is particularly unusual for two reasons. With an [[inclination]] of 47 degrees, it is has the highest-inclination orbit of any possible dwarf planet discovered thus far,{{Dubious|date=March 2014|1=Highest inclination|reason=there are 4 objects with H<7.5 that have higher inclinations. Of these, 2005 NU125 and 2006 HU122 are listed by Brown as 'possible'}} 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|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 planet]]s/[[Protoplanet|planetary embryos]] in the early Kuiper belt, and [[Orbital resonance|resonance]] interaction with an [[Formation and evolution of the Solar System#Planetary migration|outward]]-[[Planetary migration|migrating Neptune]]. The [[Kozai mechanism]] is capable of transferring the orbital eccentricity into an elevated inclination.<ref name="buffy">{{Cite journal
Considered a [[detached object]],<ref name="Swiss">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.<!-- Page 86. --></ref><ref name="LykDyn">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}}.</ref> {{mp|2004 XR|190}} is particularly unusual for two reasons. With an [[inclination]] of 47 degrees, it is had the highest-inclination orbit of any possible dwarf planet at the time of discovery,{{Dubious|date=March 2014|1=Highest inclination|reason=there are 4 objects with H<7.5 that have higher inclinations. Of these, 2005 NU125 and 2006 HU122 are listed by Brown as 'possible'}} 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|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 planet]]s/[[Protoplanet|planetary embryos]] in the early Kuiper belt, and [[Orbital resonance|resonance]] interaction with an [[Formation and evolution of the Solar System#Planetary migration|outward]]-[[Planetary migration|migrating Neptune]]. The [[Kozai mechanism]] is capable of transferring the orbital eccentricity into an elevated inclination.<ref name="buffy">{{Cite journal
| author = R. L. Allen, B. Gladman
| author = R. L. Allen, B. Gladman
| title = Discovery of a low-eccentricity, high-inclination Kuiper Belt object at 58 AU
| title = Discovery of a low-eccentricity, high-inclination Kuiper Belt object at 58 AU

Revision as of 21:25, 27 March 2014

2004 XR190
Discovery
Discovered byLynne Jones,
Brett Gladman,
John J. Kavelaars,
Jean-Marc Petit,
Joel Parker,
Phil Nicholson
Discovery dateDecember 11, 2004
Designations
Designation
2004 XR190
none
cubewano[1]
detached object
Orbital characteristics[1]
Epoch 2456200.5 (2012-Sep-30.0)
Aphelion63.93 AU
Perihelion51.60 AU (7691 Gm)
57.77 AU (8599 Gm)
Eccentricity0.1067
439.05 a (160,363 d)
276.22°
Inclination46.52°
252.352°
280.938°
Physical characteristics
Dimensions425–850 km (albedo 0.16-0.04)[2]
335–530 km (albedo 0.25–0.10)[3]
Albedo<0.25?[citation needed]
22.04[4]
4.4[1]

2004 XR190 (also written 2004 XR190) is a possible dwarf planet 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 nicknamed the object "Buffy", after the fictional vampire slayer,[citation needed] and proposed a different official name to the IAU.

Orbit

Considered a detached object,[5][6] 2004 XR190 is particularly unusual for two reasons. With an inclination of 47 degrees, it is had the highest-inclination orbit of any possible dwarf planet at the time of discovery,[<span title="there are 4 objects with H<7.5 that have higher inclinations. Of these, 2005 NU125 and 2006 HU122 are listed by Brown as 'possible' (March 2014)">dubious – discuss] 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.[2]

2004 XR190 came to aphelion around 1901.[7] Other than long-period comets, it is currently about the twelfth-most-distant known[citation needed] large body (57.6 AU)[4] in the Solar System after Eris and Dysnomia (both 96.4 AU),[8] 2007 OR10 (87.0 AU),[9] Sedna (86.3 AU),[10] 2012 VP113 (~83 AU), 2006 QH181 (82.9 AU),[11] 2006 AO101 (63.9 AU), 1999 DP8 (61.6 AU), 2004 UT10 (61.0 AU), 2003 QX113 (59.6 AU),[12] and 2007 TB418 (58.1 AU).[13]

  • The orbit of 2004 XR190. The ring in the center is Earth's orbit shown for scale. Units are in AUs.
    The orbit of 2004 XR190. The ring in the center is Earth's orbit shown for scale. Units are in AUs.
  • A side view of 2004 XR190's orbit, showing the object's high inclination. Units are AUs.
    A side view of 2004 XR190's orbit, showing the object's high inclination. Units are AUs.

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.

References

  1. ^ a b c "JPL Small-Body Database Browser: (2004 XR190)". 2011-01-10 last obs. Retrieved 2012-09-11. {{cite web}}: Check date values in: |date= (help)
  2. ^ 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. arXiv:astro-ph/0512430. Bibcode:2006ApJ...640L..83A. doi:10.1086/503098. Discovery paper. Preprint
  3. ^ E. L. Schaller and M. E. Brown (2007). "Volatile loss and retention on Kuiper belt objects" (PDF). Astrophysical Journal. 659: I.61–I.64. Bibcode:2007ApJ...659L..61S. doi:10.1086/516709. Retrieved 2008-04-02.
  4. ^ a b "AstDys 2004 XR190 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 26 May 2011. Retrieved 2011-05-16. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  5. ^ 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.
  6. ^ 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.
  7. ^ "Horizon Online Ephemeris System". California Institute of Technology, Jet Propulsion Laboratory. Retrieved 2009-03-23.
  8. ^ "AstDys (136199) Eris Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 4 June 2011. Retrieved 2011-05-05. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  9. ^ "AstDys (225088) 2007 OR10 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2011-05-05.
  10. ^ "AstDys (90377) Sedna Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2011-05-05.
  11. ^ "AstDys 2006 QH181 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2011-05-05.
  12. ^ "AstDys 2003 QX113 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 26 May 2011. Retrieved 2011-05-05. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  13. ^ "MPEC 2010-A05 Distant Minor Planets (2010 JAN. 14.0 TT)". IAU Minor Planet Center. Archived from the original on 14 January 2010. Retrieved 2010-01-02. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)

External links

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