(144897) 2004 UX10

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(144897) 2004 UX10
Discovered by AC Becker, A.W. Puckett, J. Kubica
Discovery date 20 October 2004
Orbital characteristics[3]
Epoch 2456600.5 (4 November 2013)
Aphelion 40.654 AU
Perihelion 37.568 AU
39.111 AU
Eccentricity 0.03945
244.60 yr (89339 d)
Inclination 9.53669°
Physical characteristics
Dimensions 361.0+124.2
Mass > ≈3×1019 kg
Mean density
>1.21 g/cm3[4]
>0.06 m/s2
>0.15 km/s
5–7 hours[4]
Albedo 0.141+0.044
Spectral type

(144897) 2004 UX10 is a Kuiper-belt object. It has a diameter of about 398 kilometres (247 mi)[2] and was discovered on 20 October 2004.[3] The object is a plutino (in 2:3 resonance with Neptune).[1][2][4]

It is likely a dwarf planet based on its absolute magnitude (H) and assumed albedo.[6]

Orbit and rotation[edit]

2004 UX10 is a plutino in 2:3 resonance with Neptune. This fact was established by integrating its motion over 10 million years.[2] The object is currently at 39 AU from the Sun.[5]

The rotational period of 2004 UX10 is not known but is likely to lie in the range of 5 to 7 hours.[4]

Physical properties[edit]

The size of 2004 UX10 was measured by the Herschel Space Telescope to be 361.0+124.2
.[2] The mass of the object is currently unknown but should be greater than about 3×1019 kg.[4]

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.[7]


  1. ^ a b "(144897) 2004 UX10". IAU Minor Planet Center. Retrieved 15 May 2012. 
  2. ^ a b c d e f g h i 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. 
  3. ^ a b JPL Small-Body Database Browser, Retrieved 14 November 2009
  4. ^ a b c d e 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. 
  5. ^ a b "AstDys (144897) 2004UX10 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2012-01-21. 
  6. ^ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 2011-08-25. 
  7. ^ 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. doi:10.1051/0004-6361/200912582. 

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