(416400) 2003 UZ117

Last updated
(416400) 2003 UZ117
(416400) 2003 UZ117 hst.jpg
Hubble Space Telescope image of 2003 UZ117 taken in 2010
Discovery [1] [2]
Discovered by Spacewatch
Discovery site Kitt Peak National Obs.
Discovery date24 October 2003
Designations
(416400) 2003 UZ117
2003 UZ117
TNO [1] [2]  · cubewano(?) [3]
distant [4]  · Haumea [5]
Extended [6]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 3
Observation arc 13.23 yr (4,831 days)
Aphelion 49.777 AU
Perihelion 38.325 AU
44.051 AU
Eccentricity 0.1300
292.38 yr (106,791 days)
339.93°
0° 0m 12.24s / day
Inclination 27.473°
204.72°
≈ 20 November 2032 [7]
±2 days
247.45°
Physical characteristics
Dimensions138 km [8]
371 km (derived) [9]
423 km [3]
6 h (poor) [10]
10.61±0.02 h [11]
0.07 (derived) [8]
0.09 (assumed) [3]
0.1 (assumed) [9]
BB [12]  · C [9]
4.92±0.01(R) [13]  ·4.920±0.083(R) [14]  ·5.18±0.03 [12]  ·5.22 [15]  ·5.27 [9]  ·5.27±0.02 [16]  ·5.3 [1]  ·5.4 [8]

    (416400) 2003 UZ117 (provisional designation 2003 UZ117) is a trans-Neptunian object and suspected member of the Haumea family, located in the Kuiper belt in the outermost region of the Solar System. It was discovered on 24 October 2003, by astronomers of the Spacewatch survey project at Kitt Peak Observatory, Arizona. [4] The object may also be a non-resonant cubewano. [3]

    Contents

    Orbit and physical characterization

    The orbit of 2003 UZ117 along with other Haumea family objects Haumea family orbits.png
    The orbit of 2003 UZ117 along with other Haumea family objects

    2003 UZ117 orbits the Sun at a distance of 38.3–49.8  AU once every 292 years and 5 months (semi-major axis of 44.05 AU). Its orbit has an eccentricity of 0.13 and an inclination of 27° with respect to the ecliptic. [1] Precovery images have been identified back to 2002. [4]

    Estimates for its diameter range between 138 and 423 kilometers. [3] [8] [9] Two rotational lightcurves of the object gave a rotation period of 6 and 10.61 hours with a brightness amplitude of 0.1 and 0.09 in magnitude, respectively ( U=1/2 ). [10] [11] It has a spectral type of BB, with a grey/blue rather than red color. [12]

    Origin

    Based on their common pattern of infrared water-ice absorption and the clustering of their orbital elements, the other KBOs, it appear to be collisional fragments broken off the dwarf planet Haumea. The neutral color of the spectrum of these objects in the visible range evidences a lack of complex organics on the surface of these bodies that has been studied in detail for the surface of Haumea. [5]

    See also

    Related Research Articles

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    <span class="nowrap">(55565) 2002 AW<sub>197</sub></span> Classical Kuiper belt object

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    <span class="nowrap">(208996) 2003 AZ<sub>84</sub></span> Plutino

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    <span class="nowrap">(15875) 1996 TP<sub>66</sub></span>

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    <span class="nowrap">(40314) 1999 KR<sub>16</sub></span>

    (40314) 1999 KR16 is a trans-Neptunian object on an eccentric orbit in the outermost region of the Solar System, approximately 254 kilometers (158 miles) in diameter. It was discovered on 16 May 1999, by French astronomer Audrey Delsanti and Oliver Hainaut at ESO's La Silla Observatory in northern Chile. The very reddish object is a dwarf planet candidate and has a rotation period of 11.7 hours.

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    <span class="mw-page-title-main">32532 Thereus</span>

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    <span class="nowrap">(44594) 1999 OX<sub>3</sub></span>

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    (55638) 2002 VE95 (provisional designation 2002 VE95) is a trans-Neptunian object from the outermost region of the Solar System. It was discovered on 14 November 2002, by astronomers with the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This resonant trans-Neptunian object is a member of the plutino population, locked in a 2:3 resonance with Neptune. The object is likely of primordial origin with a heterogeneous surface and a notably reddish color (RR) attributed to the presence of methanol and tholins. It has a poorly defined rotation period of 6.8 hours and measures approximately 250 kilometers (160 miles) in diameter, too small to be a dwarf planet candidate. As of 2021, it has not yet been named.

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    <span class="nowrap">(82158) 2001 FP<sub>185</sub></span>

    (82158) 2001 FP185 (provisional designation 2001 FP185) is a highly eccentric trans-Neptunian object from the scattered disc in the outermost part of the Solar System, approximately 330 kilometers in diameter. It was discovered on 26 March 2001, by American astronomer Marc Buie at Kitt Peak National Observatory in Arizona, United States.

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    References

    1. 1 2 3 4 5 "JPL Small-Body Database Browser: 416400 (2003 UZ117)" (2016-02-04 last obs.). Jet Propulsion Laboratory. Retrieved 9 December 2017.
    2. 1 2 "List Of Transneptunian Objects". Minor Planet Center. Retrieved 9 December 2017.
    3. 1 2 3 4 5 Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 9 December 2017.
    4. 1 2 3 "416400 (2003 UZ117)". Minor Planet Center. Retrieved 9 December 2017.
    5. 1 2 Pinilla-Alonso, N.; Brunetto, R.; Licandro, J.; Gil-Hutton, R.; Roush, T. L.; Strazzulla, G. (March 2009). "The surface of (136108) Haumea (2003 EL61), the largest carbon-depleted object in the trans-Neptunian belt". Astronomy and Astrophysics. 496 (2): 547–556. arXiv: 0803.1080 . Bibcode:2009A&A...496..547P. doi:10.1051/0004-6361/200809733. S2CID   15139257 . Retrieved 9 December 2017.
    6. ↑ Marc W. Buie. "Orbit Fit and Astrometric record for 416400". SwRI (Space Science Department). Retrieved 2018-02-18.
    7. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
    8. 1 2 3 4 Michael E. Brown. "How many dwarf planets are there in the outer solar system?". California Institute of Technology . Retrieved 9 December 2017.
    9. 1 2 3 4 5 "LCDB Data for (416400)". Asteroid Lightcurve Database (LCDB). Retrieved 9 December 2017.
    10. 1 2 Perna, Davide; Dotto, E.; Barucci, A.; Rossi, A.; de Bergh, C.; Doressoundiram, A.; et al. (September 2008). "Light Curves and Densities of Centaurs and Trans-Neptunian Objects from the ESO Large Program". American Astronomical Society. 40: 483. Bibcode:2008DPS....40.4708P . Retrieved 9 December 2017.
    11. 1 2 Thirouin, Audrey; Sheppard, Scott S.; Noll, Keith S.; Moskovitz, Nicholas A.; Ortiz, Jose Luis; Doressoundiram, Alain (June 2016). "Rotational Properties of the Haumea Family Members and Candidates: Short-term Variability". The Astronomical Journal. 151 (6): 20. arXiv: 1603.04406 . Bibcode:2016AJ....151..148T. doi: 10.3847/0004-6256/151/6/148 . S2CID   118510175.
    12. 1 2 3 Perna, D.; Barucci, M. A.; Fornasier, S.; DeMeo, F. E.; Alvarez-Candal, A.; Merlin, F.; et al. (February 2010). "Colors and taxonomy of Centaurs and trans-Neptunian objects". Astronomy and Astrophysics. 510: A53. arXiv: 0912.2621 . Bibcode:2010A&A...510A..53P. doi:10.1051/0004-6361/200913654. S2CID   55619450 . Retrieved 9 December 2017.
    13. ↑ Jewitt, David; Peixinho, Nuno; Hsieh, Henry H. (November 2007). "U-Band Photometry of Kuiper Belt Objects". The Astronomical Journal. 134 (5): 2046–2053. Bibcode:2007AJ....134.2046J. doi: 10.1086/522787 .
    14. ↑ Peixinho, N.; Delsanti, A.; Guilbert-Lepoutre, A.; Gafeira, R.; Lacerda, P. (October 2012). "The bimodal colors of Centaurs and small Kuiper belt objects". Astronomy and Astrophysics. 546: 12. arXiv: 1206.3153 . Bibcode:2012A&A...546A..86P. doi:10.1051/0004-6361/201219057. S2CID   55876118 . Retrieved 9 December 2017.
    15. ↑ Tegler, S. C.; Romanishin, W.; Consolmagno, G. J.; J., S. (December 2016). "Two Color Populations of Kuiper Belt and Centaur Objects and the Smaller Orbital Inclinations of Red Centaur Objects". The Astronomical Journal. 152 (6): 13. Bibcode:2016AJ....152..210T. doi: 10.3847/0004-6256/152/6/210 . S2CID   125183388.
    16. ↑ Boehnhardt, H.; Schulz, D.; Protopapa, S.; Gö; tz, C. (November 2014). "Photometry of Transneptunian Objects for the Herschel Key Program 'TNOs are Cool'". Earth. 114 (1–2): 35–57. Bibcode:2014EM&P..114...35B. doi:10.1007/s11038-014-9450-x. S2CID   122628169 . Retrieved 9 December 2017.
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