(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]
| 2005 UQ513, taken by the Palomar Observatory in 22 August 2002.[1] | |
| Discovery[2] | |
|---|---|
| Discovered by | M. E. Brown D. L. Rabinowitz C. A. Trujillo |
| Discovery date | 21 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 arc | 8474 days (23.20 yr) |
| Earliest precovery date | 15 September 1990 |
| Aphelion | 49.689 AU (7.4334 Tm) (Q) |
| Perihelion | 36.713 AU (5.4922 Tm) (q) |
| 43.201 AU (6.4628 Tm) (a) | |
| Eccentricity | 0.15018 (e) |
| 283.95 yr (103713 d) | |
| 223.93° (M) | |
| 0° 0m 12.496s / day (n) | |
| Inclination | 25.7315° (i) |
| 307.8679° (Ω) | |
| ≈ 30 July 2123[7] ±3 days | |
| 221.89° (ω) | |
| Earth MOID | 35.763 AU (5.3501 Tm) |
| Jupiter MOID | 31.568 AU (4.7225 Tm) |
| TJupiter | 5.253 |
| Physical characteristics | |
| Dimensions | 498+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] | |
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]
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]
- ^ Lowe, Andrew. “(202421) 2005 UQ513 Precovery Images”. andrew-lowe.ca.
- ^ 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.
- ^ 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.
- ^ a b “MPEC 2010-S44 : DISTANT MINOR PLANETS (2010 OCT. 11.0 TT)”. IAU Minor Planet Center. 2010-09-25. Retrieved 2011-01-26.
- ^ 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.
- ^ “AstDyS (202421) 2005UQ513 Orbital information”. Department of Mathematics, University of Pisa, Italy. Retrieved 2012-05-05.
- ^ a b JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
- ^ 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
- ^ a b “AstDyS (202421) 2005UQ513 Ephemerides”. Department of Mathematics, University of Pisa, Italy. Retrieved 2012-05-05.
- ^ 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.
- ^ 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
- ^ a b c Pinilla-Alonso, N., Licandro, J., & Lorenzi, V. (2008). Visible spectroscopy in the neighborhood of 2003 EL61 (Haumea) arXiv:0807.2670
- ^ a b c Snodgrass, C., Carry, B., Dumas, C., & Hainaut, O. (2009). Characterisation of candidate members of (136108) Haumea’s family arXiv:0912.3171