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(202421) 2005 UQ513 (provisional designation 2005 UQ513) is a cubewano with an absolute magnitude of 3.97.[3] Its spectrum has a weak signature of absorption by water ice.[10][11] Like Quaoar, it has a very red spectrum,[12][13] which indicates that its surface probably contains many complex, processed organic molecules.[12] Its light curve shows variations of Δm=0.3 mag, but no period has been determined.[13]

Classification

2005 UQ513 has a perihelion of 37.3 AU.[3] The Minor Planet Center (MPC) classifies it as a cubewano[4] while the Deep Ecliptic Survey (DES) classifies it as ScatExt (scattered-extended).[5] Although dynamically it would have been a good candidate to be a member of the Haumea collisional family, given its red spectrum, it is not.[12][13]

Distance

As of December 2018, it is currently 48.0 AU from the Sun.[9] It will come to perihelion in 2123.[7]

It has been observed 194 times over 14 oppositions with precovery images back to 1990.[3]

See also

References

  1. ^ Lowe, Andrew. "(202421) 2005 UQ513 Precovery Images". andrew-lowe.ca.
  2. ^ Brown, M.; Trujillo, C.; Rabinowitz, D.; Marsden, B. G. (2007). "2003 UY413, 2003 UZ413, 2004 NT33, 2005 CA79, 2005 CB79, 2005 UQ513". Minor Planet Electronic Circulars. 2007-R02: R02. Bibcode:2007MPEC....R...02B.
  3. ^ a b c d e f g "JPL Small-Body Database Browser: (2005 UQ513)" (2011-12-26 last obs., 12 opp). Retrieved 7 April 2016.
  4. ^ a b "MPEC 2010-S44 : DISTANT MINOR PLANETS (2010 OCT. 11.0 TT)". IAU Minor Planet Center. 2010-09-25. Retrieved 2011-01-26.
  5. ^ a b Marc W. Buie. "Orbit Fit and Astrometric record for 202421" (2012/05/06 using 59 observations). SwRI (Space Science Department). Retrieved 2012-05-05.
  6. ^ "AstDyS (202421) 2005UQ513 Orbital information". Department of Mathematics, University of Pisa, Italy. Retrieved 2012-05-05.
  7. ^ a b JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
  8. ^ a b TNOs are Cool: A survey of the trans-Neptunian region. X. Analysis of classical Kuiper belt objects from Herschel* and Spitzer observations p. 18 arXiv:1403.6309
  9. ^ a b "AstDyS (202421) 2005UQ513 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2012-05-05.
  10. ^ Ragozzine, D. & Brown, M. E. (2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328. Bibcode:2007AJ....134.2160R. doi:10.1086/522334. S2CID 8387493. Retrieved 2009-12-05.
  11. ^ Trujillo, C. A., Sheppard, S. S., & Schaller E. L. (2011). A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects arXiv:1102.1971
  12. ^ a b c Pinilla-Alonso, N., Licandro, J., & Lorenzi, V. (2008). Visible spectroscopy in the neighborhood of 2003 EL61 (Haumea) arXiv:0807.2670
  13. ^ a b c Snodgrass, C., Carry, B., Dumas, C., & Hainaut, O. (2009). Characterisation of candidate members of (136108) Haumea’s family arXiv:0912.3171

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