(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 14 November 2003[1]
Designations
MPC designation (84922) 2003 VS2
none
Plutino[3][4]
Orbital characteristics[1][3]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 8830 days (24.18 yr)
Earliest precovery date 17 September 1991
Aphelion 42.413 AU (6.3449 Tm)
Perihelion 36.456 AU (5.4537 Tm)
39.435 AU (5.8994 Tm)
Eccentricity 0.075539
247.64 yr (90451.3 d)
4.75 km/s
15.535°
0° 0m 14.328s / day
Inclination 14.777°
302.792°
114.317°
Physical characteristics
Dimensions 523.0+35.1
−34.4
 km
[5]
7.42 h (0.309 d)
7.41±0.02 h[6]
0.147+0.063
−0.043
[5]
Temperature ≈44 K
(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] 4.2[1]

(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, (84922) 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]

(84922) 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]

(84922) 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 d "JPL Small-Body Database Browser: 84922 (2003 VS2)" (2008-02-05 last obs). Retrieved 7 April 2016. 
  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:1202.3657Freely accessible. Bibcode:2012A&A...541A..93M. doi:10.1051/0004-6361/201118562. 
  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:0704.1636Freely accessible. Bibcode:2007AJ....134..787S. doi:10.1086/519072. 
  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". In Barucci, M. Antonietta; Boehnhardt, Hermann; Cruikshank, Dale P. The Solar System Beyond Neptune (pdf). University of Arizona press. pp. 161–179. arXiv:astro-ph/0702538Freely accessible. Bibcode:2008ssbn.book..161S. ISBN 0-8165-2755-5. 
  9. ^ a b Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on 2006-09-01. 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 31 August 2016. 
  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]