(84522) 2002 TC302

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(84522) 2002 TC302
Discovered byM. E. Brown,
C. A. Trujillo,
D. L. Rabinowitz(?)
Discovery date9 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 arc5574 days (15.26 yr)
Aphelion71.552 AU (10.7040 Tm)
Perihelion38.979 AU (5.8312 Tm)
55.265 AU (8.2675 Tm)
410.86 yr (150065 d)
3.93 km/s
0° 0m 8.636s / day
Earth MOID38.1784 AU (5.71141 Tm)
Jupiter MOID34.8125 AU (5.20788 Tm)
Physical characteristics
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[edit]

(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[edit]


  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[edit]