Astronomy:(202421) 2005 UQ513

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(202421) 2005 UQ513
2005uq513-20020822.gif
Precovery image of 2005 UQ513, taken by the Palomar Observatory in 22 August 2002.[1]
Discovery[3]
Discovered byM. E. Brown
D. L. Rabinowitz
C. A. Trujillo
Discovery date21 October 2005[2]
Designations
(202421) 2005 UQ513
Minor planet categoryCubewano (MPC)[4]
ScatExt (DES)[5]
Orbital characteristics[2][7]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc8474 days (23.20 yr)
Earliest precovery date15 September 1990
|{{{apsis}}}|helion}}49.689 astronomical unit|AU (7.4334 Tm) (Q)
|{{{apsis}}}|helion}}36.713 AU (5.4922 Tm) (q)
43.201 AU (6.4628 Tm) (a)
Eccentricity0.15018 (e)
Orbital period283.95 yr (103713 d)
Mean anomaly223.93° (M)
Mean motion0° 0m 12.496s / day (n)
Inclination25.7315° (i)
Longitude of ascending node307.8679° (Ω)
|{{{apsis}}}|helion}}≈ 30 July 2123[6]
±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]
Rotation period7.03 h (0.293 d)
Sidereal rotation period7.03 hr?[2]
Geometric albedo0.31+0.12
−0.065[8]
Apparent magnitude20.8 [9]
Absolute magnitude (H)3.97 [2]


(202421) 2005 UQ513 (provisional designation 2005 UQ513) is a cubewano with an absolute magnitude of 3.97.[2] 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.[2] 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.[6]

It has been observed 194 times over 14 oppositions with precovery images back to 1990.[2]

See also

  • List of gravitationally rounded objects of the Solar System

References

  1. ↑ Lowe, Andrew. "(202421) 2005 UQ513 Precovery Images". http://andrew-lowe.ca/2005uq513.htm. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 "JPL Small-Body Database Browser: (2005 UQ513)". https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2005UQ513. 
  3. ↑ 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. 
  4. ↑ 4.0 4.1 "MPEC 2010-S44 : DISTANT MINOR PLANETS (2010 OCT. 11.0 TT)". IAU Minor Planet Center. 2010-09-25. http://minorplanetcenter.org/mpec/K10/K10S44.html. 
  5. ↑ 5.0 5.1 Marc W. Buie. "Orbit Fit and Astrometric record for 202421". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/202421.html. 
  6. ↑ 6.0 6.1 JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
  7. ↑ "AstDyS (202421) 2005UQ513 Orbital information". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/astdys/index.php?pc=1.1.1&n=2005UQ513. 
  8. ↑ 8.0 8.1 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. ↑ 9.0 9.1 "AstDyS (202421) 2005UQ513 Ephemerides". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=2005UQ513. 
  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. doi:10.1086/522334. Bibcode: 2007AJ....134.2160R. https://iopscience.iop.org/article/10.1086/522334/pdf. 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. ↑ 12.0 12.1 12.2 Pinilla-Alonso, N., Licandro, J., & Lorenzi, V. (2008). Visible spectroscopy in the neighborhood of 2003 EL61 (Haumea) arXiv:0807.2670
  13. ↑ 13.0 13.1 13.2 Snodgrass, C., Carry, B., Dumas, C., & Hainaut, O. (2009). Characterisation of candidate members of (136108) Haumea’s family arXiv:0912.3171

External links



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