(84922) 2003 VS2

(84922) 2003 VS2
2003 VS2 photographed by the Hubble Space Telescope in 2005
Discovery[1]
Discovered byNEAT
Discovery sitePalomar Observatory
Discovery date14 November 2003
Designations
3A86VCM[2][3]
TNO[4] · plutino[5][6] · distant[1]
Orbital characteristics (barycentric)[7][a]
Epoch 21 November 2025 (JD 2461000.5)
Uncertainty parameter 0[4][1]
Observation arc34+ yr[4]
Earliest precovery date17 September 1991
Aphelion42.414 AU
Perihelion36.432 AU
39.423 AU
Eccentricity0.07587
247.36 yr (90,349 d)
31.436°
0° 0m 14.344s / day
Inclination14.790°
302.723°
8 March 2005[8] ± 0.11 days[4]
112.563°
Known satellites0
Physical characteristics
Dimensions(678±10) × (470±12) × (452±16) km[6]
524±7 km (volume equiv.)[6]
Mean density
1.4+1.0
−0.3 g/cm3[9]
7.4175285±0.00001 h[10]
228°[6]
+39°[6]
0.134±0.010[6]
Temperature40 K[9]
19.8[12]
4.14±0.07 (rotational avg.)[6]

(84922) 2003 VS2 is an unnamed trans-Neptunian object (TNO) in the Kuiper belt. It is a member of the plutinos, a population of TNOs in a 2:3 orbital resonance with Neptune, like Pluto. It was discovered by the Near-Earth Asteroid Tracking program at Palomar Observatory on 14 November 2003.[13] It is an elongated object with a diameter measuring 678 km (421 mi) across its longest axis to 452 km (281 mi) across its shortest.[6]

Discovery

2003 VS2 was discovered by the NASA-funded[14] Near-Earth Asteroid Tracking (NEAT) project on 14 November 2003, during routine observations of the sky at Palomar Observatory in California, United States.[1][15] The discovery observations were made using the observatory's 48-inch (1.2 m) Samuel Oschin telescope, which was equipped with a charge-coupled device camera.[13] Astronomers of the project flagged 2003 VS2 as an "interesting object" because it moved much slower than near-Earth objects that NEAT was tasked to find.[2][3] The object was listed on the Minor Planet Center's (MPC's) Near-Earth Object Confirmation Page, which prompted follow-up observations from other observatories.[16]

Within two days after the discovery of 2003 VS2, astronomers began finding precoveries of the object in older NEAT images.[13] Precoveries were first found by Maik Meyer in images from late 2002, and then by Sebastian Hönig in images from 1998, 2001, and 2002.[13][16] These extra observations allowed astronomers to determine the orbit of 2003 VS2.[16] The discovery and confirmation of 2003 VS2 was announced by the MPC on 16 November 2003.[13][16] Subsequent reports of the discovery, including those from the NEAT project, recognized 2003 VS2 as one of the largest trans-Neptunian objects found.[15][17][18]

On the day after the MPC's announcement of 2003 VS2, astronomer Reiner Stoss reported more precoveries from Palomar Observatory's Digitized Sky Survey, whose images were taken even earlier in 1991 and 1993.[18] The earliest of these precoveries was taken on 17 September 1991.[1][18] These precoveries were independently found by Andrew Lowe and Rob Matson around the same time as Stoss.[18]

Name

This object is currently known by its minor planet provisional designation 2003 VS2, which was given by the MPC upon its discovery.[13] The provisional designation encodes the object's time and order of discovery.[19] The MPC gave it the minor planet number (84922) on 4 May 2004.[20] When it was discovered, the object was initially codenamed "3A86VCM" by the NEAT project.[2][3][b] As of May 2026, it has not been named.[1] According to naming guidelines by the International Astronomical Union's Working Group for Small Bodies Nomenclature, trans-Neptunian objects classified as plutinos should be given mythological names related to the underworld.[21]: 8 

Orbit

2003 VS2 orbits the Sun with a semi-major axis of 39.4 astronomical units (AU),[a] putting it in the Kuiper belt beyond Neptune's orbit. 2003 VS2 takes 247 years to complete one orbit, which places it in a 2:3 mean-motion resonance with Neptune.[6][7] For every two revolutions it makes around the Sun, Neptune makes exactly three.[23] It is therefore a member of the plutinos, a large population of trans-Neptunian objects (TNOs) named after its largest member Pluto.[6][23]

2003 VS2 has a nearly circular orbit with a low eccentricity of 0.08. Its orbit is inclined by 14.8° with respect to the ecliptic.[7] Throughout its orbit, the object's distance from the Sun ranges from 36.4 AU at perihelion to 42.4 AU at aphelion.[a] 2003 VS2 had passed perihelion on 8 March 2005.[8] Due to gravitational perturbations by the giant planets, the orbital elements of 2003 VS2 vary over time.[5][24]: 2–3  Simulations of 2003 VS2's orbit show that in 10 million years, its semi-major axis can fluctuate between 39.1–39.8 AU, eccentricity between 0.05–0.11, and inclination between 15.4–16.8°.[5] Despite this variability, the orbit of 2003 VS2 remains stable for billions of years.[24]: 10 

Physical characteristics

Size and shape

In 2007, its diameter was initially estimated by the Spitzer Space Telescope at 725±200 km.[25] However, in 2012, this was reduced to 523.0+35.1
−34.4 km after new Herschel Space Telescope observations.[11] In 2019, 2003 VS2 was found to be ellipsoidal in shape based on stellar occultations that occurred in 2013 and 2014;[9] the light curve derived from the occultations suggests that this plutino is not in hydrostatic equilibrium and hence not a dwarf planet.[26] The dimensions of 2003 VS2 are estimated at 627.6 km × 531 km × 494.6 km, with a volume-equivalent diameter of 548.3+29.5
−44.6 km.[9]

Further observations of occultations refined the estimate to (678±10) × (470±12) × (452±16) km, with a mean diameter of 524±7 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 TNOs,[27] gives a mass estimate of about 6.5×1019 kg.

Surface

2003 VS2 (apparent magnitude 19.8) photographed with a 24-inch telescope. Surrounding stars are labeled with their apparent magnitude values for comparison.

2003 VS2 has a moderately red surface with a moderately red color indices B−V=0.93, V−R=0.59.[28] Its geometrical albedo is about 0.13.[9]

Rotation

2003 VS2 rotates with a period of approximately 7.42 hours, measured to an accuracy of 0.04 seconds.[6] It has a high light curve amplitude of 0.21±0.01, indicative of an elongated, non-spherical shape.[6]

See also

  • 90377 Sedna – a dwarf planet discovered on the same day as 2003 VS2 (14 November 2003)
  • 208996 Achlys – a large plutino and possible dwarf planet with an elongated ellipsoid shape
  • (84522) 2002 TC302 – a similarly-sized trans-Neptunian object whose shape has been characterized by stellar occultations
  • (119951) 2002 KX14 – another similarly-sized trans-Neptunian object whose shape has been characterized by stellar occultations
  • (612533) 2002 XV93 – a similarly-sized plutino discovered to have an atmosphere in stellar occultation observations

Notes

  1. 1 2 3 These orbital elements are expressed in terms of the Solar System Barycenter (SSB) as the frame of reference.[7] Due to planetary perturbations, the Sun revolves around the SSB at non-negligible distances, so heliocentric-frame orbital elements and distances (such as those given in JPL's Small-Body Database[4]) can vary on short timescales.[22]
  2. ↑ The NEAT project's six-character alphanumeric codename encodes the object's time of observation and number.[19]

References

  1. 1 2 3 4 5 6 "(84922) = 2003 VS2". Minor Planet Center. Retrieved 2 June 2026.
  2. 1 2 3 Pravdo, S. (24 November 2003). "NEAT November 2003 Interesting Objects". Near-Earth Asteroid Tracking. Jet Propulsion Laboratory. Archived from the original on 18 November 2016. Retrieved 14 June 2026.
  3. 1 2 3 4 "3A86VCM image". Near-Earth Asteroid Tracking. Jet Propulsion Laboratory. November 2003. Archived from the original on 17 January 2009. Retrieved 14 June 2026.
  4. 1 2 3 4 5 "JPL Small-Body Database Lookup: 84922 (2003 VS2)" (2025-12-28 last obs.). Jet Propulsion Laboratory. Retrieved 2 May 2026.
  5. 1 2 3 Buie, Marc W. (5 February 2008). "Orbit Fit and Astrometric record for 84922". SwRI (Space Science Department). Retrieved 23 July 2008.
  6. 1 2 3 4 5 6 7 8 9 10 11 12 13 Vara-Lubiano, M.; Benedetti-Rossi, G.; Santos-Sanz, P.; Ortiz, J. L.; Sicardy, B.; Popescu, M.; et al. (2022). "The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS2". Astronomy & Astrophysics. 663: A121. arXiv:2205.12878. Bibcode:2022A&A...663A.121V. doi:10.1051/0004-6361/202141842. S2CID 249009658.
  7. 1 2 3 4 "JPL Horizons On-Line Ephemeris for 84922 (2003 VS2) at epoch JD 2461000.5". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 2 June 2026. Solution using the Solar System Barycenter. Ephemeris Type: Elements and Center: @0)
  8. 1 2 "JPL Horizons On-Line Ephemeris for 84922 (2003 VS2) rom 2005-Mar-01 to 2005-Mar-15". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 2 June 2026. (Perihelion occurs when radial velocity or "rdot" changes from negative to positive.)
  9. 1 2 3 4 5 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). arXiv:1908.06645. doi:10.3847/1538-3881/ab3b05. S2CID 201070151.
  10. ↑ Santos-Sanz, P.; Lellouch, E.; Groussin, O.; Lacerda, P.; Muller, T.G.; Ortiz, J.L.; Kiss, C.; Vilenius, E.; Stansberry, J.; Duffard, R.; Fornasier, S.; Jorda, L.; Thirouin, A. (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. arXiv:1705.09117. Bibcode:2017A&A...604A..95S. doi:10.1051/0004-6361/201630354. S2CID 53621071.
  11. 1 2 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. S2CID 119253817.
  12. ↑ "AstDys (84922) 2003VS2 Ephemerides". Asteroids - Dynamic Site. Department of Mathematics, University of Pisa, Italy. Retrieved 2 June 2026.
  13. 1 2 3 4 5 6 Marsden, Brian G., ed. (16 November 2003). "MPEC 2003-W02 : 2003 VS2". Minor Planet Electronic Circular. 2002-V26. Minor Planet Center. Retrieved 6 January 2010.
  14. ↑ "General Information: Near-Earth Asteroid Tracking (NEAT)". Near-Earth Asteroid Tracking. Jet Propulsion Laboratory. Archived from the original on 28 December 2016. Retrieved 14 June 2026.
  15. 1 2 "Near-Earth Asteroid Tracking". Near-Earth Asteroid Tracking. Jet Propulsion Laboratory. Archived from the original on 3 December 2003. Retrieved 14 June 2026.
  16. 1 2 3 4 "Big Plutino found – '03 Major News about Minor Objects". HohmannTransfer.com. 16 November 2003. Archived from the original on 18 February 2005. Retrieved 14 June 2026.
  17. ↑ Whitehouse, David (17 November 2003). "Huge rock-ice body circles Sun". BBC. Archived from the original on 4 December 2003. Retrieved 14 June 2026.
  18. 1 2 3 4 "New 2003 VS2 precovery – '03 Major News about Minor Objects". HohmannTransfer.com. 18 November 2003. Archived from the original on 8 September 2005. Retrieved 14 June 2026.
  19. 1 2 "NEAT Object Naming System". Near-Earth Asteroid Tracking. Jet Propulsion Laboratory. Archived from the original on 6 February 2003. Retrieved 15 June 2026.
  20. ↑ "M.P.C. 51880" (PDF). Minor Planet Circulars (51880). Minor Planet Center: 416. 4 May 2004. Retrieved 2 June 2026.
  21. ↑ "Rules and Guidelines for Naming Non-Cometary Small Solar-System Bodies" (PDF). IAU Working Group for Small Bodies Nomenclature. 22 February 2025. Retrieved 2 June 2026.
  22. ↑ "JPL Horizons On-Line Ephemeris for 84922 (2003 VS2) at epochs JD 2460800.5–2461000.5". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 2 June 2026. Solution using the Sun. Ephemeris Type: Elements and Center: @sun)
  23. 1 2 "Plutinos". COSMOS - The SAO Encyclopedia of Astronomy. Swinburne University of Technology. Retrieved 2 June 2025.
  24. 1 2 Muñoz-Gutiérrez, Marco A.; Ramírez-Vargas, Sebastián; Peimbert, Antonio; Pérez-Villegas, Angeles; Petrovich, Petrovich (March 2026). "The Effect of Massive Trans-Neptunian Objects in the Long-term Evolution and Leakage Rates of Neptune's 3:2 and 2:1 Mean Motion Resonances". The Astronomical Journal. 171 (3): 177. arXiv:2503.03900. Bibcode:2026AJ....171..177M. doi:10.3847/1538-3881/ae3e51.
  25. ↑ 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. (eds.). The Solar System Beyond Neptune. University of Arizona press. pp. 161–179. arXiv:astro-ph/0702538. Bibcode:2008ssbn.book..161S. ISBN 978-0-8165-2755-7.
  26. ↑ 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.
  27. ↑ 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)". Icarus. 334: 30–38. Bibcode:2019Icar..334...30G. doi:10.1016/j.icarus.2018.12.037. S2CID 126574999.
  28. ↑ Tegler, Stephen C. (1 February 2007). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on 1 September 2006. Retrieved 30 December 2009.
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