(144897) 2004 UX10

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(144897) 2004 UX10
Discovered by A. C. Becker
A. W. Puckett
J. Kubica
Discovery site Apache Point Obs.
Discovery date 20 October 2004
MPC designation (144897) 2004 UX10
TNO[2] · plutino[3]
Orbital characteristics[2]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 2
Observation arc 62.37 yr (22,781 days)
Aphelion 40.461 AU
Perihelion 37.270 AU
38.865 AU
Eccentricity 0.0410
242.30 yr (88,500 days)
0° 0m 14.76s / day
Inclination 9.5390°
Physical characteristics
Dimensions 361+124
398±39 km[3][4]
Mass > ≈ 3×1019 kg
Mean density
> 1.21 g/cm3[5]
Equatorial surface gravity
> 0.06 m/s2
Equatorial escape velocity
> 0.15 km/s
5.68±0.05 h[5]
B–V =0.95±0.02
V–R = 0.58±0.05[3]

(144897) 2004 UX10 is a Kuiper-belt object. It has a diameter of about 360 kilometres (220 mi)[3] and was discovered by Andrew Becker, Andrew Puckett and Jeremy Kubica on 20 October 2004 at Apache Point Observatory in Sunspot, New Mexico.[2] The object is a plutino (in 2:3 resonance with Neptune).[3][5]

It is likely a dwarf planet based on its absolute magnitude (H) and assumed albedo.[7]

Orbit and rotation[edit]

(144897) 2004 UX10 is a plutino in 2:3 resonance with Neptune. This fact was established by integrating its motion over 10 million years.[3] The object is currently at 39 AU from the Sun.[6]

The rotational period of (144897) 2004 UX10 is 5.68 h.[2]

Physical properties[edit]

The size of (144897) 2004 UX10 was measured by the Herschel Space Telescope to be 361+124
.[3] The mass of the object is currently unknown but should be greater than about 3×1019 kg.[5]

(144897) 2004 UX10 has a moderately red slope in the visible spectral range. Its visible spectrum does not show any features, although there is a small departure from the linearity near 0.8 μm.[8]

See also[edit]


  1. ^ "List Of Transneptunian Objects". Minor Planet Center. Retrieved 22 August 2016.
  2. ^ a b c d e "144897 (2004 UX10)". JPL Small-Body Database Browser (2008-08-23 last obs). Retrieved 7 April 2016.
  3. ^ a b c d e f g h i j Mommert, Michael; Harris, A. W.; Kiss, C.; Pál, A.; Santos-Sanz, P.; Stansberry, J.; Delsanti, A.; Vilenius, E.; Müller, T. G.; Peixinho, N.; Lellouch, E.; Szalai, N.; Henry, F.; Duffard, R.; Fornasier, S.; Hartogh, P.; Mueller, M.; Ortiz, J. L.; Protopapa, S.; Rengel, M.; Thirouin, A. (May 2012). "TNOs are cool: A survey of the trans-Neptunian region—V. Physical characterization of 18 Plutinos using Herschel-PACS observations". Astronomy & Astrophysics. 541: A93. arXiv:1202.3657. Bibcode:2012A&A...541A..93M. doi:10.1051/0004-6361/201118562.
  4. ^ a b "LCDB Data for (144897)". Asteroid Lightcurve Database (LCDB). Retrieved 6 September 2016.
  5. ^ a b c d Thirouin, A.; Ortiz, J. L.; Duffard, R.; Santos-Sanz, P.; Aceituno, F. J.; Morales, N. (2010). "Short-term variability of a sample of 29 trans-Neptunian objects and Centaurs". Astronomy & Astrophysics. 522: A93. arXiv:1004.4841. Bibcode:2010A&A...522A..93T. doi:10.1051/0004-6361/200912340.
  6. ^ a b "AstDys (144897) 2004UX10 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2012-01-21.
  7. ^ 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 2011-10-18. Retrieved 2011-08-25.
  8. ^ Fornasier, S.; Barucci, M. A.; de Bergh, C.; Alvarez-Candal, A.; Demeo, F.; Merlin, F.; Perna, D.; Guilbert, A.; Delsanti, A.; Dotto, E.; Doressoundiram, A. (2009). "Visible spectroscopy of the new ESO large programme on trans-Neptunian objects and Centaurs: Final results". Astronomy and Astrophysics. 508 (1): 457–465. arXiv:0910.0450. Bibcode:2009A&A...508..457F. doi:10.1051/0004-6361/200912582.

External links[edit]