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(455502) 2003 UZ413

2003 UZ413
2003uz413-19961014.gif
Precovery image of 2003 UZ413 taken by the Siding Spring Observatory in 1996.[1]
Discovery[2]
Discovered byM. E. Brown
D. L. Rabinowitz
C. A. Trujillo
Discovery date21 October 2003
Designations
MPC designation2003 UZ413
TNO[3] · plutino[4][5][a]
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 2
Observation arc63.25 years (23103 days)
Earliest precovery date29 July 1954
Aphelion47.968 AU (7.1759 Tm)
Perihelion30.241 AU (4.5240 Tm)
39.104 AU (5.8499 Tm)
Eccentricity0.22667
244.54 yr (89317.3 d)
113.43°
0° 0m 14.51s / day
Inclination12.04911°
135.930°
145.00°
Physical characteristics
Dimensions367–820 km[3][6][7][b]
536 km[8][c]
680 km[9][d]
Mass300×1018 kg[e]
Mean density
2.29–3.00 > ρ >0.72 g/cm3[10]
2.64 g/cm3[9]
4.13±0.05 h[10][11]
4.14 h[3]
0.07[9]
0.08[8]
0.05–0.25 (assumed)[6][7]
BB taxon (blue/neutral)[9][12][f]
V−R=0.46±0.06
R−I=0.37±0.06[12]
20.98[13]
4.3[3][10]
4.38+0.08
−0.07
,[12]
4.4[14]
4.7[8]

(455502) 2003 UZ413, also written as 2003 UZ413, is a trans-Neptunian object (TNO) with an absolute magnitude of 4.38.[12] It is in a 2:3 orbital resonance with Neptune, thus it is classified as a plutino.[4] It is likely large enough to be a dwarf planet. It was given the minor planet number 455502 on 22 February 2016.[1]

It has been observed 79 times over 15 oppositions, with precovery images back to 27 July 1954.[3]

Orbit and rotation

2003 UZ413 is in a 2:3 resonance with Neptune, which means that when it makes two revolutions around the Sun, Neptune makes exactly three.[4]

The object rotates very fast. In fact, with a period of about 4.13 hours, it is the fastest rotator known in the Kuiper belt after Haumea.[10][11]

Physical characteristics

The size of 2003 UZ413 is not known, but a reasonable estimate is around 600 kilometres (370 mi).[3][7][9][8][g] This estimate puts it on the borderline between the 2nd ("highly likely") and 3rd ("likely") classes in astronomer Michael Brown's five-level system of classifying the probability that an object is a dwarf planet, although he himself only estimates its size at 536 km, therefore more towards the lower end of the "likely" group.[8]

Given its rapid rotation, it must have a density higher than 0.72 g/cm3.[10] Stable Jacobi ellipsoids with an axis ratio of a/b1.13±0.03, as implied by its light-curve amplitude of Δm = 0.13±0.03, exist for densities in the range of 2.29−3.00 g/cm3.[10] The Johnston's Archive settles on 2.64 g/cm3,[9] the centre of the latter range; for a 600 km equivalent spheroid body, this would equate to a mass of approximately 3.0×1020 kg. The relatively high estimated density (in stark contrast to many similarly sized TNOs) [15] increases the chance that the object has no internal porosity and has collapsed into hydrostatic equilibrium (a requirement of being certified as a Dwarf Planet), but confirmation of this hypothesis requires observations to refine the size and light curve details, preferably with determination of the orbit of any satellite that may exist.

In visible light, this object is neutral or slightly red in color and has a flat, featureless reflectance spectrum.[11]

Notes

  1. ^ Buie page actually says 3:2 resonance... thus, also "Plutino"
  2. ^ using assumed albedo of 0.25 to 0.05, and 4.3 absolute magnitude as per JPL/MPC; using 4.38 magnitude as per Perna et al (2010) gives a ~3.3% smaller estimate, i.e. 356-791 km
  3. ^ using 0.08 albedo and 4.7 magnitude
  4. ^ using 0.07 albedo; if given to nearest km, size calculates back to a source magnitude of approx 4.340 to 4.345
  5. ^ very approximate figure, assuming equivalent spherical diameter of ≈600 km and density ≈2.64 g/cc3
  6. ^ equivalent to V-I=0.75±0.06, B-V=0.68±0.06 and V-R=0.39±0.05
  7. ^ mean of the Johnston's Archive and Mike Brown figures plus centrepoint of the wider range derived from JPL/MPC magnitude, rounded to 2sf

References

  1. ^ a b "(455502) 2003 UZ413 Precovery Images". Retrieved 28 April 2019.
  2. ^ Brown, M.; Trujillo, C.; Rabinowitz, D.; Marsden, B. G. (2007-09-01). "2003 UY413, 2003 UZ413, 2004 NT33, 2005 CA79, 2005 CB79, 2005 UQ513". Minor Planet Electronic Circulars: 02. Bibcode:2007MPEC....R...02B. MPEC 2007-R02.
  3. ^ a b c d e f g "JPL Small-Body Database Browser: (2003 UZ413)" (last observation: 2017-10-29). Retrieved 19 August 2019.
  4. ^ a b c Marsden, B. G. (2008-07-17). "Distant Minor Planets". Minor Planet Electronic Circulars. Bibcode:2008MPEC....O...05B. MPEC 2008-O05. Retrieved 3 December 2010.
  5. ^ Marc W. Buie (2015-09-24). "Orbit Fit and Astrometric record for 2003 UZ413". SwRI (Space Science Department). Archived from the original on 2015-09-23. Retrieved 2019-08-19.
  6. ^ a b Dan Bruton. "Conversion of Absolute Magnitude to Diameter for Minor Planets". Stephen F. Austin State University, College of Sciences and Mathematics, Department of Physics, Engineering and Astronomy. Archived from the original on 23 July 2011. Retrieved 15 August 2019.
  7. ^ a b c "Absolute Magnitude (H)". NASA/JPL. Archived from the original on 1 September 2008. Retrieved 2019-08-19.
  8. ^ a b c d e Prof. Mike Brown (30 May 2019). "How many dwarf planets are there in the outer solar system?". Mike Brown's Planets. Caltech Division of Geological and Planetary Sciences. Archived from the original on 31 May 2019. Retrieved 19 August 2019.
  9. ^ a b c d e f William Robert Johnston. "List of known trans-Neptunian objects". Johnston's Archive. Retrieved 2019-08-19.
  10. ^ a b c d e f Perna, D.; Dotto, E.; Barucci, M. A.; Rossi, A.; Fornasier, S.; de Bergh, C. (21 October 2009). "Rotations and densities of trans-Neptunian objects". Astronomy & Astrophysics. 508 (1): 451–455. Bibcode:2009A&A...508..451P. doi:10.1051/0004-6361/200911970. Retrieved 1 June 2019.
  11. ^ a b c 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" (PDF). Astronomy and Astrophysics. 508 (1): 457–465. arXiv:0910.0450. Bibcode:2009A&A...508..457F. doi:10.1051/0004-6361/200912582.
  12. ^ a b c d Perna, D.; Barucci, M.A.; Fornasier, S.; et al. (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.
  13. ^ "2003 UZ413 Ephemerides". Asteroids Dynamic Site. Archived from the original on 2019-08-19. Retrieved 2019-08-19.
  14. ^ "2003 UZ413 Summary". Asteroids Dynamic Site. Archived from the original on 2019-08-19. Retrieved 2019-08-19.
  15. ^ W.M. Grundy, K.S. Noll, M.W. Buie, S.D. Benecchi, D. Ragozzine & H.G. Roe, 'The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ((229762) 2007 UK126)', Icarus (forthcoming, available online 30 March 2019) DOI: 10.1016/j.icarus.2018.12.037,

External links