Astronomy:(144897) 2004 UX10

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Short description: Kuiper Belt object


(144897) 2004 UX10
Discovery[1]
Discovered byA. C. Becker
A. W. Puckett
J. Kubica
Discovery siteApache Point Obs.
Discovery date20 October 2004
Designations
(144897) 2004 UX10
Minor planet categoryTNO[2] · cubewano[3][4]
Orbital characteristics[2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 2
Observation arc65.21 yr (23,818 days)
|{{{apsis}}}|helion}}40.591 AU
|{{{apsis}}}|helion}}37.152 AU
38.871 AU
Eccentricity0.0442
Orbital period242.35 yr (88,520 days)
Mean anomaly102.254°
Mean motion0° 0m 14.76s / day
Inclination9.5316°
Longitude of ascending node147.90°
149.15°
Physical characteristics
Dimensions361+124
−94 km[5]
398±39 km[5][6]
Mass> ≈ 3×1019 kg
Mean density> 1.21 g/cm3[7]
Equatorial surface gravity
> 0.06 m/s2
Equatorial escape velocity
> 0.15 km/s
Rotation period5.68±0.05 h[7]
Geometric albedo0.141+0.044
−0.031[5]
B–V =0.95±0.02
V–R = 0.58±0.05[5]
C[6]
Apparent magnitude20.6[8]
Absolute magnitude (H)4.75±0.16[5]
4.4[2]


(144897) 2004 UX10 (provisional designation 2004 UX10) is a Kuiper-belt object. It has a diameter of about 360 kilometres (220 mi)[5] 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 classified as a cubewano.[3][4] It is near a 2:3 resonance with Neptune.[5][7]

It is estimated by astronomer Michael E. Brown to likely be a dwarf planet based on its presumed size, calculated from its absolute magnitude (H) and assumed albedo.[9]

Orbit and rotation

Based on an integration of its motion over 10 million years, (144897) 2004 UX10 has been classified as a classical Kuiper belt object (cubewano).[3] It is near a 2:3 resonance with Neptune.[5] The object is currently at 39 AU from the Sun.[8]

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

Physical properties

The size of (144897) 2004 UX10 was measured by the Herschel Space Telescope to be 361+124
−94 km.[5] The mass of the object is currently unknown but should be greater than about 3×1019 kg.[7]

(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.[10]

See also

References

  1. ↑ "List Of Transneptunian Objects". Minor Planet Center. https://www.minorplanetcenter.net/iau/lists/TNOs.html. Retrieved 22 August 2016. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 "144897 (2004 UX10)". JPL Small-Body Database Browser. 13 July 2019. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=144897. Retrieved 3 November 2019. 
  3. ↑ 3.0 3.1 3.2 Buie, M. (3 November 2019). "Orbit Fit and Astrometric record for 144897". SwRI (Space Science Department). https://www.boulder.swri.edu/~buie/kbo/astrom/144897.html. Retrieved 3 November 2019. 
  4. ↑ 4.0 4.1 Johnston, W. R. (13 July 2019). "List of Known Trans-Neptunian Objects". http://www.johnstonsarchive.net/astro/tnoslist.html. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 Mommert, Michael; Harris, A. W.; Kiss, C.; Pál, A.; Santos-Sanz, P.; Stansberry, J.; Delsanti, A.; Vilenius, E. et al. (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. doi:10.1051/0004-6361/201118562. Bibcode: 2012A&A...541A..93M. 
  6. ↑ 6.0 6.1 "LCDB Data for (144897)". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=144897%7C. Retrieved 6 September 2016. 
  7. ↑ 7.0 7.1 7.2 7.3 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. doi:10.1051/0004-6361/200912340. Bibcode: 2010A&A...522A..93T. 
  8. ↑ 8.0 8.1 "AstDys (144897) 2004UX10 Ephemerides". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=144897. Retrieved 2012-01-21. 
  9. ↑ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. http://www.gps.caltech.edu/~mbrown/dps.html. Retrieved 2011-08-25. 
  10. ↑ Fornasier, S.; Barucci, M. A.; de Bergh, C.; Alvarez-Candal, A.; Demeo, F.; Merlin, F.; Perna, D.; Guilbert, A. et al. (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. Bibcode: 2009A&A...508..457F. 

External links



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