(84922) 2003 VS2

Last updated

(84922) 2003 VS2
84922-2003vs2 hst.jpg
Hubble Space Telescope image of 2003 VS2 taken in 2005
Discovery [1]
Discovered by NEAT (644)
Discovery date14 November 2003 [2]
Designations
(84922) 2003 VS2
none
Plutino [3] [4]
Orbital characteristics [2] [3]
Epoch 13 January 2016 (JD  2457400.5)
Uncertainty parameter 3
Observation arc 8830 days (24.18 yr)
Earliest precovery date17 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)
Average orbital speed
4.75 km/s
15.535°
0° 0m 14.328s / day
Inclination 14.777°
302.792°
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 density
1.4+1.0
−0.3 g/cm3 [6]
7.4175285±0.00001  h [8]
7.41±0.02 h [9]
0.134±0.01 [5]
Temperature ≈44 K
19.7 [10]
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. [1] 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]

Contents

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. [2]

(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 2003VS2-mag20.jpg
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. TheTransneptunians Color Distribution.svg
Colours of the TNOs plus Phoebe, Pholus, Triton and Mars. Mars and Triton are not to scale.

See also

Related Research Articles

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<span class="nowrap">(455502) 2003 UZ<sub>413</sub></span>

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

(126154) 2001 YH140, also written as (126154) 2001 YH140, is a resonant trans-Neptunian object discovered on 18 December 2001, by American astronomers Chad Trujillo and Michael Brown at the Palomar Observatory in California. It measures approximately 345 kilometers in diameter.

(55638) 2002 VE95, prov. designation: 2002 VE95, is a trans-Neptunian object from the outermost region of the Solar System. It was discovered on 14 November 2002, by astronomers with the Near-Earth Asteroid Tracking program at the Palomar Observatory in California, United States. This resonant trans-Neptunian object is a member of the plutino population, locked in a 2:3 resonance with Neptune. The object is likely of primordial origin with a heterogeneous surface and a notably reddish color (RR) attributed to the presence of methanol and tholins. It has a poorly defined rotation period of 6.8 hours and measures approximately 250 kilometers (160 miles) in diameter, too small to be a dwarf planet candidate. As of 2021, it has not yet been named.

<span class="nowrap">(612533) 2002 XV<sub>93</sub></span>

(612533) 2002 XV93, also written as 2002 XV93, is a trans-Neptunian object (TNO) with an absolute magnitude of 5.4. A 2:3 orbital resonance with Neptune makes it a plutino.

(144897) 2004 UX10 is a Kuiper-belt object. It has a diameter of about 360 kilometres (220 mi) and was discovered by Andrew Becker, Andrew Puckett and Jeremy Kubica on 20 October 2004 at Apache Point Observatory in Sunspot, New Mexico. The object is classified as a cubewano. It is near a 2:3 resonance with Neptune.

<span class="mw-page-title-main">Ilmarë</span> Moon of 174567 Varda

Ilmarë, or Varda I, full designation 174567 Varda I Ilmarë, is the single known natural satellite of the Kuiper belt object 174567 Varda. It was discovered by Keith Noll et al. in 2009, at a separation of about 0.12 arcsec, using discovery images taken by the Hubble Space Telescope on 26 April 2009, and reported in 2011. At approximately 326 km in diameter (about 45% that of its primary), it is the fourth or fifth-largest known moon of a trans-Neptunian object, after Pluto I Charon, Eris I Dysnomia, Orcus I Vanth and very possibly Haumea I Hiʻiaka. Assuming that Ilmarë has the same albedo and density as Varda, Ilmarë would constitute approximately 8.4% of the system's mass, approximately 2.2×1019 kg.

References

  1. 1 2 Marsden, Brian G. (16 November 2003). "MPEC 2003-W02 : 2003 VS2". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. Retrieved 6 January 2010.
  2. 1 2 3 "JPL Small-Body Database Browser: 84922 (2003 VS2)" (2008-02-05 last obs). Retrieved 7 April 2016.
  3. 1 2 3 Buie, Marc W. (5 February 2008). "Orbit Fit and Astrometric record for 84922". SwRI (Space Science Department). Retrieved 23 July 2008.
  4. 1 2 "MPEC 2006-X45 : Distant Minor Planets". Minor Planet Center & Tamkin Foundation Computer Network. 21 December 2006. Archived from the original on 28 August 2008. Retrieved 23 July 2008.
  5. 1 2 3 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. arXiv: 2205.12878 . Bibcode:2022A&A...663A.121V. doi:10.1051/0004-6361/202141842. S2CID   249009658.
  6. 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.
  7. 1 2 3 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.
  8. 1 2 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.
  9. 1 2 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. S2CID   56247384.
  10. ↑ "AstDys (84922) 2003VS2 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 27 March 2012. Retrieved 7 December 2009.
  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)
  12. ↑ 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.
  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" (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.
  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)". Icarus. 334: 30–38. Bibcode:2019Icar..334...30G. doi:10.1016/j.icarus.2018.12.037. S2CID   126574999.
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