(84522) 2002 TC302

(84522) 2002 TC302
Discovery[1]
Discovered by M. E. Brown,
C. A. Trujillo,
D. L. Rabinowitz(?)
Discovery date October 9, 2002
Designations
MPC designation (84522) 2002 TC302

SDO[2]

2:5 resonance[3][4]
Orbital characteristics[5]
Epoch July 23, 2010 (JD 2455400.5)
Aphelion 71.870 AU
(10,752 Gm)
Perihelion 39.199 AU
(5,864.1 Gm)
55.535 AU
(8,307.86 Gm)
Eccentricity 0.29415
413.86 yr
(151,162 d)
3.93 km/s
318.100°
Inclination 34.976°
23.823°
85.975°
Physical characteristics
Dimensions 584.1+105.6
−88.0[6]
5.41 h[7]
Albedo 0.115+0.047
−0.033[6]
Spectral type
 (red) B−V=1.03;
V−R=0.67[8]
20.5 (opposition)[9]
3.78±0.53[5]

    (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

    2002 TC302 has an absolute magnitude (H) of 3.78.[5] It has an estimated diameter of 584.1+105.6
    −88.0     km    .[6] Using the Spitzer Space Telescope, it was previously estimated to have a diameter of 1145+337
    −325     km    ,[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, 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 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]

    Orbit

    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, 2002 TC302 comes to opposition in late October of each year at an apparent magnitude of 20.5.[9]

    Resonance

    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 2002 TC302 relative to Neptune being held stationary
    Animated

    The 2:5 resonance motion of 2002 TC302 (red) and the 2:3 resonance of Pluto (grey). Neptune is held stationary.

    Precovery

    It has been observed 76 times over nine years.[5]

    See also

    References

    1. ↑ 1.0 1.1 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. ↑ 2.0 2.1 "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 2008-09-19.
    3. ↑ 3.0 3.1 3.2 3.3 Marc W. Buie (2007-09-16). "Orbit Fit and Astrometric record for 84522". SwRI (Space Science Department). Retrieved 2008-09-19.
    4. ↑ 4.0 4.1 "MPEC 2009-C70 :Distant Minor Planets (2009 FEB. 28.0 TT)". Minor Planet Center. 2009-02-10. Retrieved 2009-03-05.
    5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 "JPL Small-Body Database Browser: 84522 (2002 TC302)" (last observation:2009-10-25). Retrieved 2011-01-02.
    6. ↑ 6.0 6.1 6.2 6.3 S. Fornasier, E. Lellouch, T. Müller, P. Santos-Sanz, P. Panuzzo, C. Kiss, T. Lim, M. Mommert, D. Bockelée-Morvan, E. Vilenius, J. Stansberry, G.P. Tozzi, S. Mottola, A. Delsanti, J. Crovisier, R. Duffard, F. Henry, P. Lacerda, A. Barucci, & A. Gicquel (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.
    7. ↑ 7.0 7.1 Short-term variability of 10 trans-Neptunian objects
    8. ↑ Tegler, Stephen C. (2006-01-26). "Kuiper Belt Object Magnitudes and Surface Colors". Retrieved 2006-11-05.
    9. ↑ 9.0 9.1 "(84522) 2002 TC302". Minor Planet Center. 2010-07-23. Retrieved 2010-10-24.
    10. ↑ 10.0 10.1 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].
    11. ↑ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 2013-11-30.
    12. ↑ Stevge Preston's Asteroid Occultation Updates item; accessed 22 February 2013

    External links

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