Astronomy:(84922) 2003 VS2

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Short description: Trans-Neptunian object


(84922) 2003 VS2
84922-2003vs2 hst.jpg
Hubble Space Telescope image of 2003 VS2 taken in 2005
Discovery[2]
Discovered byNEAT (644)
Discovery date14 November 2003[1]
Designations
(84922) 2003 VS2
none
Minor planet categoryPlutino[3][4]
Orbital characteristics[1][3]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc8830 days (24.18 yr)
Earliest precovery date17 September 1991
|{{{apsis}}}|helion}}42.413 astronomical unit|AU (6.3449 Tm)
|{{{apsis}}}|helion}}36.456 AU (5.4537 Tm)
39.435 AU (5.8994 Tm)
Eccentricity0.075539
Orbital period247.64 yr (90451.3 d)
Average Orbital speed4.75 km/s
Mean anomaly15.535°
Mean motion0° 0m 14.328s / day
Inclination14.777°
Longitude of ascending node302.792°
114.317°
Physical characteristics
Dimensions(678±10) × (470±12) × (452±16) km[5]
Mean diameter
  • 524±7 km[5]
  • 548.3+29.5
    −44.6     km    [6]
  • 523.0+35.1
    −34.4     km    [7]
Mean density1.4+1.0
−0.3 g/cm3[6]
Rotation period7.4175285±0.00001 h[8]
Sidereal rotation period7.41±0.02 h[9]
Geometric albedo0.134±0.01[5]
Physics≈44 K
Apparent magnitude19.7[10]
Absolute magnitude (H)4.11±0.38[8]


(84922) 2003 VS2 is a trans-Neptunian object discovered by the Near Earth Asteroid Tracking program on 14 November 2003.[2] Like Pluto, it is in a 2:3 orbital resonance with Neptune[3][4] and is thus a plutino. Analysis of light-curve suggests that it is not a dwarf planet.[11]

Orbit and rotation

Like Pluto, (84922) 2003 VS2 is locked in the 3:2 mean-motion resonance with Neptune, although its orbit is both less inclined and significantly less eccentric than Pluto's.[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.[9]

Physical characteristics

(84922) 2003 VS2 has a moderately red surface with a moderately red color indices B−V=0.93, V−R=0.59.[12] Its geometrical albedo is about 0.13.[6]

In 2007, its diameter was initially estimated by the Spitzer Space Telescope at 725±200 km.[13] However, in 2012, this was reduced to 523.0+35.1
−34.4 km after new Herschel Space Telescope observations.[7] In 2019, 2003 VS2 was found to be ellipsoidal in shape based on stellar occultations that occurred in 2013 and 2014;[6] the light curve derived from the occultations suggests that this plutino is not in hydrostatic equilibrium and hence not a dwarf planet.[14] The dimensions of 2003 VS2 are estimated at 627.6 km × 531 km × 494.6 km, with a volume-equivalent diameter 548.3+29.5
−44.6 km.[6] 2003 VS2 has no known satellite that can be used to directly determine its mass, but assuming a density of 1 g/cm3, typical of mid size TNO's,[15] gives a mass estimate of about 7.5×1019 kg.

2003 VS2 (apparent magnitude 19.8) as viewed with a 24" telescope
Colours of the TNOs plus Phoebe, Pholus, Triton and Mars. Mars and Triton are not to scale.

See also

  • Sedna, another large trans-Neptunian object discovered the same day (14 November 2003)

References

  1. ↑ 1.0 1.1 1.2 "JPL Small-Body Database Browser: 84922 (2003 VS2)". https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=84922. Retrieved 7 April 2016. 
  2. ↑ 2.0 2.1 Marsden, Brian G. (2003-11-16). "MPEC 2003-W02 : 2003 VS2". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. http://www.cfa.harvard.edu/mpec/K03/K03W02.html. Retrieved 2010-01-06. 
  3. ↑ 3.0 3.1 3.2 Buie, Marc W. (2008-02-05). "Orbit Fit and Astrometric record for 84922". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/84922.html. Retrieved 2008-07-23. 
  4. ↑ 4.0 4.1 "MPEC 2006-X45 : Distant Minor Planets". Minor Planet Center & Tamkin Foundation Computer Network. 2006-12-21. http://cfa-www.harvard.edu/iau/mpec/K06/K06X45.html. Retrieved 2008-07-23. 
  5. ↑ 5.0 5.1 5.2 Vara-Lubiano, M. et al. (2022). "The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS2". Astronomy & Astrophysics 663: A121. doi:10.1051/0004-6361/202141842. Bibcode: 2022A&A...663A.121V. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Benedetti-Rossi, Gustavo; Santos-Sanz, P.; Ortiz, J. L.; Assafin, M.; Sicardy, B.; Morales, N. (2019). "The trans-Neptunian object (84922) 2003 VS2 through stellar occultations". The Astronomical Journal 158 (4). doi:10.3847/1538-3881/ab3b05. 
  7. ↑ 7.0 7.1 7.2 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. 
  8. ↑ 8.0 8.1 Santos-Sanz, P.; Lellouch, E.; Groussin, O.; Lacerda, P.; Muller, T.G.; Ortiz, J.L.; Kiss, C.; Vilenius, E. et al. (August 2017). ""TNOs are Cool": A survey of the trans-Neptunian region XII. Thermal light curves of Haumea, 2003 VS2 and 2003 AZ84 with Herschel/PACS". Astronomy & Astrophysics 604 (A95): 19. doi:10.1051/0004-6361/201630354. Bibcode: 2017A&A...604A..95S. 
  9. ↑ 9.0 9.1 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. doi:10.1086/519072. Bibcode: 2007AJ....134..787S. 
  10. ↑ "AstDys (84922) 2003VS2 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=84922. Retrieved 2009-12-07. 
  11. ↑ Tancredi, Gonzalo (2009). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Proceedings of the International Astronomical Union Symposium S263 5: 173–185. doi:10.1017/S1743921310001717. Bibcode: 2010IAUS..263..173T.  (Dwarf Planet & Plutoid Headquarters)
  12. ↑ Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". http://www.physics.nau.edu/~tegler/research/survey.htm. Retrieved 2009-12-30. 
  13. ↑ 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. University of Arizona press. pp. 161–179. ISBN 978-0-8165-2755-7. Bibcode: 2008ssbn.book..161S. http://www.lpi.usra.edu/books/ssbn2008/7017.pdf. 
  14. ↑ Benedetti-Rossi, Gustavo; Santos-Sanz, Pablo; Ortiz, Jose Luis; Assafin, Marcelo; Sicardy, Bruno; Vieira-Martins, Roberto; Braga-Ribas, Felipe (2019). "Three Stellar Occultations by the Plutino Object (84922) 2003 VS2". Epsc-DPS Joint Meeting 2019 2019: EPSC-DPS2019-435. Bibcode: 2019EPSC...13..435B. 
  15. ↑ Grundy, W.M.; Noll, K.S.; Buie, M.W.; Benecchi, S.D.; Ragozzine, D.; Roe, H.G. (2019). "The mutual orbit, mass, and density of transneptunian binary Gǃkúnǁ'hòmdímà (229762 2007 UK126)" (in en). Icarus 334: 30–38. doi:10.1016/j.icarus.2018.12.037. Bibcode: 2019Icar..334...30G. 

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