(84522) 2002 TC302

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(84522) 2002 TC302
Discovered by M. E. Brown,
C. A. Trujillo,
D. L. Rabinowitz(?)
Discovery date 9 October 2002
MPC designation (84522) 2002 TC302
2:5 resonance[3][4]
Orbital characteristics[5]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 5574 days (15.26 yr)
Aphelion 71.552 AU (10.7040 Tm)
Perihelion 38.979 AU (5.8312 Tm)
55.265 AU (8.2675 Tm)
Eccentricity 0.29469
410.86 yr (150065 d)
Average orbital speed
3.93 km/s
0° 0m 8.636s / day
Inclination 35.107°
Earth MOID 38.1784 AU (5.71141 Tm)
Jupiter MOID 34.8125 AU (5.20788 Tm)
Physical characteristics
Dimensions 584.1+105.6
5.41 h (0.225 d)[7]
(red) B−V=1.03;
20.5 (opposition)[9]

(84522) 2002 TC302 is a red 2:5 resonant[3] trans-Neptunian object (TNO) discovered on October 9, 2002 by Mike Brown's team at the Palomar Observatory.[1]

Physical characteristics

(84522) 2002 TC302 has an absolute magnitude (H) of 3.78.[5] It has an estimated diameter of 584.1+105.6
.[6] Using the Spitzer Space Telescope, it was previously estimated to have a diameter of 1145+337
,[10] which would have made it one of the largest possible dwarf planets. This overestimation was due to insufficient motion to allow for a good sky subtraction and because it was very close to a brighter background object.[6] Brown noted that the Spitzer measurement involved a very large potential error and that the object would likely be smaller, making its chances of it being a dwarf planet "likely" rather than "near certainty", in his opinion.[11]

It was predicted that on 30 November 2013, (84522) 2002 TC302 might occult a star for slightly less than a minute.[12] However, the possibility to observe this occultation was judged as small. The precise duration that a Solar System object occults a star provides a precise way to determine its diameter, if observed from multiple locations.

The red spectra suggests that (84522) 2002 TC302 has very little fresh ice on its surface.[10]

Comparison of 2002 TC302 with selected other trans-Neptunian objects

Its rotational period is most likely 5.41 h, and it has a light-curve amplitude of 0.04±0.01 mag.[7]


(84522) 2002 TC302 will come to perihelion in 2058.[5] Its perihelion (minimum distance from the Sun) of 39.1 AU[5] is about the same as Pluto's semi-major axis (average distance from the Sun). It is classified as a scattered disc object.[2][3]

Given the long orbit that TNOs have around the Sun, (84522) 2002 TC302 comes to opposition in late October of each year at an apparent magnitude of 20.5.[9]


Both the Minor Planet Center (MPC) and the Deep Ecliptic Survey (DES) show this probable dwarf planet to be in a 2:5 resonance with Neptune.[3][4] Due to the resonance, it completes two orbits for every five orbits of Neptune.

As of 2009, it is the largest likely dwarf planet that is known to be in a non-plutino resonance with Neptune. Plutinos are objects in 2:3 mean-motion resonance with Neptune. For every two orbits that a plutino makes, Neptune makes three.

Still frame
A still frame showing the motion of (84522) 2002 TC302 relative to Neptune being held stationary.
Dwarf2002TC302 46000y.gif
The 2:5 resonance motion of (84522) 2002 TC302 (red) and the 2:3 resonance of Pluto (grey). Neptune is held stationary.


It has been observed 76 times back to August 5, 2000.[5]

See also


  1. ^ a b Marsden, Brian G. (2002-11-07). "MPEC 2002-V26 : 2002 TC302". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. Retrieved 2010-01-06.
  2. ^ a b "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 2008-09-19.
  3. ^ a b c d Marc W. Buie (2007-09-16). "Orbit Fit and Astrometric record for 84522". SwRI (Space Science Department). Retrieved 2008-09-19.
  4. ^ a b "MPEC 2009-C70 :Distant Minor Planets (2009 FEB. 28.0 TT)". Minor Planet Center. 2009-02-10. Retrieved 2009-03-05.
  5. ^ a b c d e f "JPL Small-Body Database Browser: 84522 (2002 TC302)" (last observation:2009-10-25). Retrieved 7 April 2016.
  6. ^ a b c d Fornasier, S.; Lellouch, E.; Müller, T.; Santos-Sanz, P.; et al. (July 2013). "TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of 9 bright targets at 70–500 µm" (PDF). Astronomy & Astrophysics. 555. doi:10.1051/0004-6361/201321329. A15.
  7. ^ a b Thirouin, A.; Ortiz, J.L.; Campo Bagatin, A.; Pravec, P.; et al. (21 August 2012). "Short-term variability of 10 trans-Neptunian objects" (PDF). Monthly Notices of the Royal Astronomical Society. 424 (4): 3156–3177. doi:10.1111/j.1365-2966.2012.21477.x.
  8. ^ Tegler, Stephen C. (2006-01-26). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on 2006-09-01. Retrieved 2006-11-05.
  9. ^ a b "(84522) 2002 TC302". Minor Planet Center. 2010-07-23. Retrieved 2010-10-24.
  10. ^ a b John Stansberry; Will Grundy; Mike Brown; Dale Cruikshank; et al. (2007). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". arXiv:astro-ph/0702538.
  11. ^ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 31 August 2016.
  12. ^ Stevge Preston's Asteroid Occultation Updates item Archived 2013-10-30 at the Wayback Machine.; accessed 22 February 2013

External links

  • TNO 2002 TC302, Image of the Month (January 2003)
  • (84522) 2002 TC302 at the JPL Small-Body Database
    • Close approach · Discovery · Ephemeris · Orbit diagram · Orbital elements · Physical parameters
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