2010 GB174
Orbits of 2010 GB174 (dark blue) and other scattered/detached objects, along with hypothetical Planet Nine on the right
Discovery
Discovery date12 April 2010
Designations
Designation
2010 GB174
detached object
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Observation arc2.64 years
Earliest precovery date26 June 2009
Aphelion
  • 649 AU (barycentric)[2]
  • 693±53 AU (Q)
Perihelion48.7±0.3 AU
  • 349 AU (barycentric)[3][2]
  • 371±29 AU (a)
Eccentricity0.869±0.01
  • 6500 yr (barycentric)[2]
  • 7150±827 yr
3.22°±0.4°
0° 0m 0.575s / day
Inclination21.54°
130.6° (Ω)
≈ 1951-Aug-20[4]
347.8°±0.4° (ω)
Physical characteristics
Dimensions
  • 223 km (based on assumed albedo)[5]
  • 130–300 km[1][6]
Albedo0.08 (assumed)[5]
25.2[7]
6.6[1]

2010 GB174 is a detached object, discovered on 12 April 2010 on data taken at the Canada France Hawaii Telescope as part of the Next Generation Virgo Cluster Survey.[8][9] It never gets closer than 48.5 AU from the Sun (about the outer edge of the Kuiper belt). Its large eccentricity strongly suggests that it was gravitationally scattered onto its current orbit. It is, like all detached objects, outside the current influence of Neptune, so how it got its current orbit is unknown. 2010 GB174 has the third highest Tisserand parameter relative to Jupiter of any Trans-Neptunian object, after Sedna and 2012 VP113. It has not been observed since 2015.[1] It comes to opposition in late March each year in the constellation of Virgo.

Precovery images have been found back to 26 June 2009.[1]

It reached perihelion (closest approach to the Sun) in mid-1951[4] and has moved beyond 70 AU in September 2014.[7] It is possibly a dwarf planet.[5]

Comparison

The orbits of Sedna, 2012 VP113, Leleākūhonua, and other very distant objects along with the predicted orbit of Planet Nine. The three sednoids (pink) along with the red-colored extreme trans-Neptunian object (eTNO) orbits are suspected to be aligned with the hypothetical Planet Nine while the blue-colored eTNO orbits are anti-aligned. The highly elongated orbits colored brown include centaurs and damocloids with large aphelion distances over 200 AU.

See also

References

  1. ^ a b c d e "JPL Small-Body Database Browser: (2010 GB174)". Archived from the original on 26 June 2013. Retrieved 24 January 2016.
  2. ^ a b c Horizons output. "Barycentric Osculating Orbital Elements for 2010 GB174". Retrieved 20 September 2021. (Ephemeris Type:Elements and Center:@0)
  3. ^ Malhotra, Renu; Volk, Kathryn; Wang, Xianyu (2016). "Corralling a distant planet with extreme resonant Kuiper belt objects". The Astrophysical Journal Letters. 824 (2): L22. arXiv:1603.02196. Bibcode:2016ApJ...824L..22M. doi:10.3847/2041-8205/824/2/L22. S2CID 118422279.
  4. ^ a b "Horizons Batch for 2010 GB174 on 1951-Aug-20" (Perihelion occurs when rdot flips from negative to positive). JPL Horizons. Retrieved 20 September 2021. (JPL#6/Soln.date: 2021-Apr-15)
  5. ^ a b c Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 18 October 2011. Retrieved 16 February 2014.
  6. ^ "ABSOLUTE MAGNITUDE (H)". NASA/JPL. Archived from the original on 2 March 2001. Retrieved 27 May 2013.
  7. ^ a b "AstDyS 2010 GB174 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 28 March 2014.
  8. ^ Chen, Ying-Tung; Kavelaars, J. J.; Gwyn, Stephen; Ferrarese, Laura; Côté, Patrick; Jordán, Andrés; Suc, Vincent; Cuillandre, Jean-Charles; Ip, Wing-Huen (1 September 2013). "Discovery of a New Member of the Inner Oort Cloud from the Next Generation Virgo Cluster Survey". The Astrophysical Journal. 775 (1): L8. arXiv:1308.6041. Bibcode:2013ApJ...775L...8C. doi:10.1088/2041-8205/775/1/L8. ISSN 0004-637X.
  9. ^ "Home". NGVS. Retrieved 11 January 2022.

External links

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