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(202421) 2005 UQ513

(202421) 2005 UQ513
Precovery image of 2005 UQ513, taken by the Palomar Observatory in 22 August 2002.[1]
Discovery[2]
Discovered byM. E. Brown
D. L. Rabinowitz
C. A. Trujillo
Discovery date21 October 2005[3]
Designations
(202421) 2005 UQ513
Cubewano (MPC)[4]
ScatExt (DES)[5]
Orbital characteristics[3][6]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc8474 days (23.20 yr)
Earliest precovery date15 September 1990
Aphelion49.689 AU (7.4334 Tm) (Q)
Perihelion36.713 AU (5.4922 Tm) (q)
43.201 AU (6.4628 Tm) (a)
Eccentricity0.15018 (e)
283.95 yr (103713 d)
223.93° (M)
0° 0m 12.496s / day (n)
Inclination25.7315° (i)
307.8679° (Ω)
≈ 30 July 2123[7]
±3 days
221.89° (ω)
Earth MOID35.763 AU (5.3501 Tm)
Jupiter MOID31.568 AU (4.7225 Tm)
TJupiter5.253
Physical characteristics
Dimensions498+63
−75 km[8]
7.03 h (0.293 d)
7.03 hr?[3]
0.31+0.12
−0.065[8]
20.8 [9]
3.97 [3]

(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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