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(90568) 2004 GV9

From Wikipedia, the free encyclopedia

(90568) 2004 GV9
2004-gv9 hst.jpg
Hubble Space Telescope image of 2004 GV9, taken on March 2010
Discovered byNEAT
Discovery date13 April 2004
MPC designation(90568) 2004 GV9
Cubewano (MPC)[2]
Extended (DES)[3]
Orbital characteristics[4]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 2
Observation arc22031 days (60.32 yr)
Earliest precovery date21 December 1954
Aphelion45.618 AU (6.8244 Tm)
Perihelion38.7281 AU (5.79364 Tm)
42.173 AU (6.3090 Tm)
273.88 yr (100034 d)
0° 0m 12.956s / day
Earth MOID37.7917 AU (5.65356 Tm)
Jupiter MOID33.6786 AU (5.03825 Tm)
Physical characteristics
Dimensions680±34 km[5]
5.86 h (0.244 d)
5.86 h[4]
4.25±0.04,[5] 4.0[4]

(90568) 2004 GV9 (also written (90568) 2004 GV9) is a trans-Neptunian object that was discovered on April 13, 2004 by NEAT.[1] It has been listed as a cubewano by the Minor Planet Center.[2]

Brown calculates that is very likely a dwarf planet.[9] A diameter of 680±34 km has been calculated from combined observations of the Herschel and Spitzer space telescopes.[5] Tancredi notes that light-curve-amplitude analysis shows only small deviations, suggesting that (90568) 2004 GV9 could be a spheroid with small albedo spots and hence a dwarf planet.[10] However, its low albedo suggests it has never been resurfaced and thus is unlikely to have planetary geology.

It has been observed forty-seven times, with precovery images back to 1954.[4]


  1. ^ a b Spahr, Timothy B. (2004-04-14). "MPEC 2004-G32 : 2004 GV9". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. Retrieved 2010-01-06.
  2. ^ a b "MPEC 2009-R09 : Distant Minor Planets (2009 SEPT. 16.0 TT)". IAU Minor Planet Center. 2009-09-04. Retrieved 2009-10-04.
  3. ^ Marc W. Buie. "Orbit Fit and Astrometric record for 90568" (2004-06-09 using 46 of 47 observations). SwRI (Space Science Department). Retrieved 2009-10-04.
  4. ^ a b c d "JPL Small-Body Database Browser: 90568 (2004 GV9)" (2011-04-11 last obs). Retrieved 7 April 2016.
  5. ^ a b c d Vilenius, E.; Kiss, C.; Mommert, M.; et al. (2012). ""TNOs are Cool": A survey of the trans-Neptunian region VI. Herschel/PACS observations and thermal modeling of 19 classical Kuiper belt objects". Astronomy & Astrophysics. 541: A94. arXiv:1204.0697. Bibcode:2012A&A...541A..94V. doi:10.1051/0004-6361/201118743.
  6. ^ Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on 2006-09-01. Retrieved 2009-12-30.
  7. ^ David L. Rabinowitz; Bradley E. Schaefer; Martha W. Schaefer; Suzanne W. Tourtellotte (2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". The Astronomical Journal. 136: 1502–1509. arXiv:0804.2864. Bibcode:2008AJ....136.1502R. doi:10.1088/0004-6256/136/4/1502.
  8. ^ "AstDys (90568) 2004GV9 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2009-10-06.
  9. ^ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 30 August 2016.
  10. ^ 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

This page was last edited on 11 May 2019, at 04:04
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