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(19308) 1996 TO66 (also written (19308) 1996 TO66) is a trans-Neptunian object that was discovered in 1996 by Chadwick Trujillo, David Jewitt and Jane Luu. Until 20000 Varuna was discovered, it was the second-largest known object in the Kuiper belt, after Pluto.

(19308) 1996 TO66
Hubble Space Telescope image of 1996 TO66 taken in 2005
Discovery
Discovered by
Discovery date12 October 1996
Designations
MPC designation
(19308) 1996 TO66
Minor planet category
  • Haumeid
  • TNO
  • intermittent 11:19 resonance?[1]
Orbital characteristics[2]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc7322 days (20.05 yr)
Aphelion48.375 AU (7.2368 Tm)
Perihelion37.939 AU (5.6756 Tm)
Semi-major axis
43.157 AU (6.4562 Tm)
Eccentricity0.12090
Orbital period (sidereal)
283.52 yr (103,555 d)
Mean anomaly
137.16°
Mean motion
0° 0m 12.515s / day
Inclination27.4948°
Longitude of ascending node
355.2889°
Argument of perihelion
239.07°
Earth MOID37.0117 AU (5.53687 Tm)
Jupiter MOID33.0091 AU (4.93809 Tm)
Physical characteristics
Dimensions
  • 200 km (assuming a Haumea-like albedo of 0.7)[3]
  • (<902km)[4]
Synodic rotation period
7.92 h (0.330 d)
Sidereal rotation period
7.92 h[2]
Geometric albedo
0.7 (assumed)
Temperature~43 K
Spectral type
  • Neutral
  • B−V = 0.68, V−R = 0.39[5]
  • B−V = 0.74, V−R = 0.38[6]
Absolute magnitude (H)
4.5

    Origin


    Main article: Haumea family
    1996 TO66 (center top) imaged by the NTT at La Silla in 1998. Other objects are elongated due to the 4-hour-exposure. The horizontal streak is from a geostationary satellite.
    1996 TO66 (center top) imaged by the NTT at La Silla in 1998. Other objects are elongated due to the 4-hour-exposure. The horizontal streak is from a geostationary satellite.

    Based on their common pattern of IR water-ice absorptions, neutral visible spectrum[7] and the clustering of their orbital elements, the other KBOs (24835) 1995 SM55, (55636) 2002 TX300, (120178) 2003 OP32 and (145453) 2005 RR43 all appear to be collisional fragments broken off of the dwarf planet Haumea.


    Orbit


    The eccentricity of 1996 TO66 varies between ca. 0.110 and 0.125 every 2 million years, with additional variations on the order of ± 0.01 on much shorter time scales. It is in an intermittent 19:11 resonance with Neptune. The resonance breaks every 2 million years when the eccentricity is highest and the orbit is closest to Neptune.[1]


    References


    1. D. Ragozzine; M. E. Brown (4 September 2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328. Bibcode:2007AJ....134.2160R. doi:10.1086/522334.
    2. "JPL Small-Body Database Browser: 19308 (1996 TO66)" (2003-10-18 last obs). Retrieved 5 April 2016.
    3. Dan Bruton. "Conversion of Absolute Magnitude to Diameter for Minor Planets". Department of Physics & Astronomy (Stephen F. Austin State University). Archived from the original on 23 March 2010. Retrieved 27 December 2009.
    4. Grundy, W. M. (2004). "Diverse albedos of small trans-neptunian objects". Icarus. 176: 22. arXiv:astro-ph/0502229. Bibcode:2005Icar..176..184G. doi:10.1016/j.icarus.2005.01.007.
    5. Snodgrass, Carry; Dumas, Hainaut (16 December 2009). "Characterisation of candidate members of (136108) Haumea's family". Astronomy and Astrophysics. arXiv:0912.3171. Bibcode:2010A&A...511A..72S. doi:10.1051/0004-6361/200913031.
    6. Tegler, Stephen C. (1 February 2007). "Kuiper Belt Object Magnitudes and Surface Colors". Archived from the original on 1 September 2006. Retrieved 7 November 2006.
    7. Pinilla-Alonso, N.; Licandro, J.; Gil-Hutton, R.; Brunetto, R. (June 2007). "The water ice rich surface of (145453) 2005 RR43: a case for a carbon-depleted population of TNOs?". Astronomy and Astrophysics. 468 (1): L25. arXiv:astro-ph/0703098. Bibcode:2007A&A...468L..25P. doi:10.1051/0004-6361:20077294.



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    На других языках

    [de] (19308) 1996 TO66

    (19308) 1996 TO66 ist ein großes transneptunisches Objekt, das bahndynamisch als erweitertes Scattered Disk Object (DO) oder als Cubewano (CKBO) sowie als Mitglied der Haumea-Familie eingestuft wird. Aufgrund seiner Größe ist der Asteroid ein Zwergplanetenkandidat.
    - [en] (19308) 1996 TO66

    [ru] (19308) 1996 TO66

    (19308) 1996 TO66 — транснептуновый объект. Находится в резонансе 11:19 с Нептуном[7]. Он был обнаружен в 1996 году Чадом Трухильо, Дэвидом Джуиттом и Джейн Лу. Первоначально был принят за очень крупный объект диаметром более 902 км[8].


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