(84922) 2003 VS2

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(84922) 2003 VS2
2003VS2-mag20.jpg
2003 VS2 (apparent magnitude 19.8) as viewed with a 24" telescope
Discovery[2]
Discovered by NEAT (644)
Discovery date November 14, 2003[1]
Designations
MPC designation (84922) 2003 VS2
none
Minor planet category Plutino[3][4]
Orbital characteristics[1][3]
Epoch December 31, 2006 (JD 2454100.5)
Aphelion 42.104 AU (6298.735 Gm)
Perihelion 36.427 AU (5449.350 Gm)
39.266 AU (5874.042 Gm)
Eccentricity 0.072
246.05 a (89,870.237 d)
4.75 km/s
3.987°
Inclination 14.798°
302.682°
112.586°
Physical characteristics
Dimensions 523.0+35.1
−34.4
 km
[5]
7.41±0.02 h[6]
Albedo 0.147+0.063
−0.043
[5]
Temperature ≈44 K
Spectral type
(moderately red) B−V= 0.93±0.02
V−R= 0.59±0.02[5]
19.7[7]
4.10±0.38[5]
4.4[8]
4.73±0.02[9]

(84922) 2003 VS2 is a trans-Neptunian object discovered by the Near Earth Asteroid Tracking program on November 14, 2003.[2] Like Pluto, it is in a 2:3 orbital resonance with Neptune,[3][4] giving it the orbital properties of a plutino. Mike Brown's website lists it as highly likely a dwarf planet.[10] However, Brown assumed that VS2 was much bigger than it really is, and the light-curve analysis has questioned whether it would truly be in the hydrostatic equilibrium.[11]

Orbit and rotation[edit]

Like Pluto, 2003 VS2 is locked in the 3:2 mean motion resonance with Neptune, although its orbit is significantly less eccentric than Pluto's. It also has slightly smaller orbital inclination.[1]

2003 VS2 has a significant light-curve amplitude of 0.21±0.01. The most likely value of the rotation period is 7.41±0.02 h.[6]

Physical characteristics[edit]

2003 VS2 has a moderately red surface with a moderately red color indexes B-V=0.93, V-R=0.59.[9] Its geometrical albedo is about 15%.[5]

In 2007, its diameter was initially estimated by the Spitzer Space Telescope at 725±200 km.[8] However, in 2012, this was reduced to 523.0+35.1
−34.4
 km
after new Herschel Space Telescope observations.[5] The latter measurement is considered more reliable. Assuming a Pluto-like density of 2 g/cm3, one can obtain a mass estimate of about 1.5×1020 kg.

Colours of the TNOs plus Phoebe, Pholus, Triton and Mars. Mars and Triton are not to scale.

References[edit]

  1. ^ a b c "JPL Small-Body Database Browser: 84922 (2003 VS2)". 2008-02-05 last obs. Retrieved 2008-07-23.  Check date values in: |date= (help)
  2. ^ a b Marsden, Brian G. (2003-11-16). "MPEC 2003-W02 : 2003 VS2". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. Retrieved 2010-01-06. 
  3. ^ a b c Buie, Marc W. (2008-02-05). "Orbit Fit and Astrometric record for 84922". SwRI (Space Science Department). Retrieved 2008-07-23. 
  4. ^ a b "MPEC 2006-X45 : Distant Minor Planets". Minor Planet Center & Tamkin Foundation Computer Network. 2006-12-21. Archived from the original on 28 August 2008. Retrieved 2008-07-23. 
  5. ^ a b c d e f 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.  edit
  6. ^ a b Sheppard, Scott S. (August 2007). "Light Curves of Dwarf Plutonian Planets and other Large Kuiper Belt Objects: Their Rotations, Phase Functions, and Absolute Magnitudes". The Astronomical Journal 134 (2): 787–798. arXiv:0704.1636. Bibcode:2007AJ....134..787S. doi:10.1086/519072.  edit
  7. ^ "AstDys (84922) 2003VS2 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2009-12-07. 
  8. ^ a b Stansberry, John; Grundy, Will; Brown, Mike; Cruikshank, Dale; Spencer, John; Trilling, David; Margot, Jean-Luc (2008). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope" (pdf). In Barucci, M. Antonietta; Boehnhardt, Hermann; Cruikshank, Dale P. The Solar System Beyond Neptune. University of Arizona press. pp. 161–179. arXiv:astro-ph/0702538. ISBN 0-8165-2755-5. 
  9. ^ a b Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". Retrieved 2009-12-30. 
  10. ^ Brown, Michael E.. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 2011-08-25. 
  11. ^ Tancredi, Gonzalo (2009). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Proceedings of the International Astronomical Union Symposium S263 5: 173–185. Bibcode:2010IAUS..263..173T. doi:10.1017/S1743921310001717.  (Dwarf Planet & Plutoid Headquarters)

External links[edit]