(144897) 2004 UX10

(144897) 2004 UX10
Discovery [1]
Discovered by A. C. Becker
A. W. Puckett
J. M. Kubica
Discovery site APO
Discovery date 20 October 2004
Designations
MPC designation (144897) 2004 UX10
TNO, plutino[2]
Orbital characteristics [3]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 22781 days (62.37 yr)
Aphelion 40.471 AU (6.0544 Tm)
Perihelion 37.332 AU (5.5848 Tm)
38.901 AU (5.8195 Tm)
Eccentricity 0.040340
242.64 yr (88623.2 d)
00405°/d
97.676°
0° 0m 14.624s / day
Inclination 9.5397°
148.08°
149.12°
Earth MOID 36.3183 AU (5.43314 Tm)
Jupiter MOID 32.2009 AU (4.81719 Tm)
Physical characteristics
Dimensions 361+124
−94 km[2]
Mass > ≈ 3×1019 kg
Mean density
 > 1.21 g/cm3[4]
Equatorial surface gravity
 > 0.06 m/s2
Equatorial escape velocity
 > 0.15 km/s
5.68 h (0.237 d)
5–7 hours[4]
0.141+0.044
−0.031[2]
0.95±0.02
0.58±0.05[2]
20.6[5]
4.75±0.16[2]
4.7[3]

    (144897) 2004 UX10 is a Kuiper-belt object. It has a diameter of about 360 kilometres (220 mi)[2] and was discovered by Andrew Becker, Andrew Puckett and Jeremy Kubica on 20 October 2004 at Apache Point Observatory in Sunspot, New Mexico.[3] The object is a plutino (in 2:3 resonance with Neptune).[2][4]

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

    Orbit and rotation

    (144897) 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 (144897) 2004 UX10 is not known but is likely to lie in the range of 5 to 7 hours.[4]

    Physical properties

    The size of (144897) 2004 UX10 was measured by the Herschel Space Telescope to be 361+124
    −94     km    .[2] The mass of the object is currently unknown but should be greater than about 3×1019 kg.[4]

    (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.[7]

    See also

    References

    1. ↑ "List Of Transneptunian Objects". Minor Planet Center. Retrieved September 2015.
    2. 1 2 3 4 5 6 7 8 9 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. 1 2 3 "144897 (2004 UX10)". JPL Small-Body Database Browser (2008-08-23 last obs). Retrieved 7 April 2016.
    4. 1 2 3 4 5 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. 1 2 "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. arXiv:0910.0450. Bibcode:2009A&A...508..457F. doi:10.1051/0004-6361/200912582.

    External links

    This article is issued from Wikipedia - version of the Friday, April 08, 2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.