(90568) 2004 GV9

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(90568) 2004 GV9
Discovery[1]
Discovered by NEAT
Discovery date 13 April 2004
Designations
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 arc 22031 days (60.32 yr)
Earliest precovery date 21 December 1954
Aphelion 45.618 AU (6.8244 Tm)
Perihelion 38.7281 AU (5.79364 Tm)
42.173 AU (6.3090 Tm)
Eccentricity 0.081681
273.88 yr (100034 d)
34.6030°
0° 0m 12.956s / day
Inclination 21.9718°
250.6142°
293.200°
Earth MOID 37.7917 AU (5.65356 Tm)
Jupiter MOID 33.6786 AU (5.03825 Tm)
Physical characteristics
Dimensions 680±34 km[5]
5.86 h (0.244 d)
5.86 h[4]
0.077+0.0084
−0.0077
[5]
B−V=0.95,
V−R=0.52[6]
B0−V0=0.843[7]
19.9[8]
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]

It 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] 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]

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

References[edit]

  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:1204.0697Freely accessible. 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:0804.2864Freely accessible. 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[edit]