(90568) 2004 GV9
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(90568) 2004 GV9
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Discovery[1]
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| Discovered by | NEAT |
| Discovery date | April 13, 2004 |
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Designations
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| MPC designation | (90568) 2004 GV9 |
| Minor planet category |
Cubewano (MPC)[2] Extended (DES)[3] |
| Epoch January 30, 2005 (JD2453400.5) | |
| Aphelion | 45.7403 AU |
| Perihelion | 38.7336 AU |
| Semi-major axis | 42.2369 AU |
| Eccentricity | 0.0830 |
| Orbital period | 274.5028 y |
| Mean anomaly | 20.3717° |
| Inclination | 21.9702° |
| Longitude of ascending node | 250.6281° |
| Argument of perihelion | 292.9643° |
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Physical characteristics
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| Dimensions | 677±70 km[5] |
| Mass | 1.1–5.0×1020 kg[6] |
| Sidereal rotation period |
5.86 h[4] |
| Albedo | 0.08±0.02[5] |
| Spectral type | B-V=0.95, V-R=0.52[7] B0-V0=0.843[8] |
| Apparent magnitude | 19.9[9] |
| Absolute magnitude (H) | 3.9[4] |
(90568) 2004 GV9 (also written (90568) 2004 GV9) is a trans-Neptunian object. It was discovered on April 13, 2004 by NEAT.[1] It is currently listed as a cubewano by the Minor Planet Center.[2]
It is very likely a dwarf planet. The Spitzer Space Telescope has estimated it to have a diameter of 677±70 km.[5] Light-curve-amplitude analysis shows only small deviations, suggesting that 2004 GV9 could be a spheroid with small albedo spots and hence a dwarf planet.[10]
It has been observed 47 times with precovery images back to 1954.[4]
References
- ^ a b Spahr, Timothy B. (2004-04-14). "MPEC 2004-G32 : 2004 GV9". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. http://www.cfa.harvard.edu/mpec/K04/K04G32.html. Retrieved 2010-01-06.
- ^ a b "MPEC 2009-R09 : Distant Minor Planets (2009 SEPT. 16.0 TT)". IAU Minor Planet Center. 2009-09-04. http://www.cfa.harvard.edu/mpec/K09/K09R09.html. Retrieved 2009-10-04.
- ^ Marc W. Buie (2004-06-09 using 46 of 47 observations). "Orbit Fit and Astrometric record for 90568". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/90568.html. Retrieved 2009-10-04.
- ^ a b c d "JPL Small-Body Database Browser: 90568 (2004 GV9)". 2004-06-09 last obs. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=90568. Retrieved 2009-08-28.
- ^ a b c John Stansberry, Will Grundy, Mike Brown, Dale Cruikshank, John Spencer, David Trilling, Jean-Luc Margot (2007). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". arXiv:astro-ph/0702538 [astro-ph].
- ^ (Radius of 303.5 km and density of 0.97 = 1.1×1020 kg mass. Radius of 373.5 km and density of 2.3 = 5.0×1020 kg mass)
- ^ 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.
- ^ David L. Rabinowitz, Bradley E. Schaefer, Martha W. Schaefer, Suzanne W. Tourtellotte (2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". arXiv:0804.2864.
- ^ "AstDys (90568) 2004GV9 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=90568. Retrieved 2009-10-06.
- ^ Tancredi, G., & Favre, S. (2008) Which are the dwarfs in the Solar System?. Depto. Astronomía, Fac. Ciencias, Montevideo, Uruguay; Observatorio Astronómico Los Molinos, MEC, Uruguay. Retrieved 10-08-2011
External links
- Orbital simulation from JPL (Java) / Ephemeris
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