(84922) 2003 VS2
From Wikipedia, the free encyclopedia
VS2 (apparent magnitude 19.8) as viewed with a 24" telescope
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Discovery[2]
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| Discovered by | NEAT (644) |
| Discovery date | November 14, 2003[1] |
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Designations
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| MPC designation | (84922) 2003 VS2 |
| Alternate name(s) | none |
| Minor planet category |
Plutino[3][4] |
| Epoch December 31, 2006 (JD 2454100.5) | |
| Aphelion | 6298.735 Gm (42.104 AU) |
| Perihelion | 5449.350 Gm (36.427 AU) |
| Semi-major axis | 5874.042 Gm (39.266 AU) |
| Eccentricity | 0.072 |
| Orbital period | 89870.237 d (246.05 a) |
| Average orbital speed | 4.75 km/s |
| Mean anomaly | 3.987° |
| Inclination | 14.798° |
| Longitude of ascending node | 302.682° |
| Argument of perihelion | 112.586° |
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Physical characteristics
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| Dimensions | 725+188 −199 km[5][6] |
| Mass | ≈4×1020? kg[7] |
| Mean density | 2.0? g/cm³ |
| Equatorial surface gravity | 0.1778? m/s² |
| Escape velocity | 0.3362? km/s |
| Sidereal rotation period |
7.41 ± 0.02 h[8] |
| Albedo | 0.036–0.106[5] |
| Temperature | ~44 K |
| Spectral type | (moderately red) B-V=0.93, V-R=0.59[9] |
| Apparent magnitude | 19.7[10] |
| Absolute magnitude (H) | 3.97[1] 4.4[5] |
(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 automatically updated website lists it as a highly likely dwarf planet.[11] But light curve analysis has questioned whether it would truly qualify as a dwarf planet.[12]
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[edit] Orbit and rotation
Like Pluto, 2003 VS2 is locked in the 3:2 mean motion resonance with Neptune, although its orbit is significantly less eccentric less than Pluto's is. It also has slightly smaller orbital inclination.[1]
The most likely value of the rotation period of this object is 7.41 ± 0.02 hours.[8]
[edit] Physical characteristics
With a moderately red color index (B-V=0.93, V-R=0.59),[9] and a Spitzer size estimate of 725 ± 200 km,[5] this plutino is also a dwarf-planet candidate. At around a size of 400 km, trans-Neptunian objects are expected to be spherical.[13]
[edit] References
- ^ a b c d "JPL Small-Body Database Browser: 84922 (2003 VS2)". 2008-02-05 last obs. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=84922. Retrieved 2008-07-23.
- ^ a b 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.
- ^ a b c Marc W. Buie (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.
- ^ 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. http://web.archive.org/web/20080828191100/http://cfa-www.harvard.edu/iau/mpec/K06/K06X45.html. Retrieved 2008-07-23.
- ^ a b c d John Stansberry, Will Grundy, Mike Brown, Dale Cruikshank, John Spencer, David Trilling, Jean-Luc Margot (2008). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". In M. Antonietta Barucci, Hermann Boehnhardt, Dale P. Cruikshank (pdf). The Solar System Beyond Neptune. University of Arizona press. pp. 161–179. arXiv:astro-ph/0702538. ISBN 0-8165-2755-5. http://www.lpi.usra.edu/books/ssbn2008/7017.pdf.
- ^ Wm. Robert Johnston (22 April 2008). "List of Known Trans-Neptunian Objects". Johnston's Archive. Archived from the original on 16 December 2006. http://web.archive.org/web/20061216155220/http://johnstonsarchive.net/astro/tnoslist.html. Retrieved 2006-12-14.
- ^ Using the 2007 Spitzer spherical radius of 362.5 km; volume of a sphere * an assumed density of 2 g/cm³ yields a mass (m=d*v) of 3.99E+20 kg
- ^ a b Sheppard, Scott S. (2006). "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. Bibcode 2007AJ....134..787S. doi:10.1086/519072.
- ^ a b 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.
- ^ "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.
- ^ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. http://www.gps.caltech.edu/~mbrown/dps.html. Retrieved 2011-08-25.
- ^ 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)
- ^ Mike Brown. "The Dwarf Planets". Archived from the original on 29 January 2008. http://web.archive.org/web/20080129195021/http://web.gps.caltech.edu/~mbrown/dwarfplanets/. Retrieved 2008-01-20.
[edit] External links
- Orbital simulation from JPL (Java) / Ephemeris
- Huge rock-ice body circles Sun (Palomar Photo)
- 2003 VS2 precovery (18 Nov. '03 Major News about Minor Objects)
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