(19308) 1996 TO66

(19308) 1996 TO66

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.
Discovery
Discovered by Chadwick Trujillo
David Jewitt
Jane Luu
Discovery date 12 October 1996
Designations
MPC designation (19308) 1996 TO66
TNO
weak eighth-order 11:19 resonance? [1]
Orbital characteristics [2]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 7322 days (20.05 yr)
Aphelion 48.375 AU (7.2368 Tm)
Perihelion 37.939 AU (5.6756 Tm)
43.157 AU (6.4562 Tm)
Eccentricity 0.12090
283.52 yr (103555 d)
137.16°
0° 0m 12.515s / day
Inclination 27.4948°
355.2889°
239.07°
Earth MOID 37.0117 AU (5.53687 Tm)
Jupiter MOID 33.0091 AU (4.93809 Tm)
Physical characteristics
Dimensions 200 km (assuming a Haumea-like albedo of 0.7) [3]
(<902km) [4]
7.92 h (0.330 d)
7.92 h [2]
0.7 (assumed)
(Neutral)
B−V=0.68, V−R=0.39 [5]
B−V=0.74; V−R=0.38 [6]
4.5

    (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.

    Origin

    Main article: Haumea family

    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.

    References

    1. ↑ D. Ragozzine; M. E. Brown (2007-09-04). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61". The Astronomical Journal. 134 (6): 2160–2167. arXiv:0709.0328Freely accessible. Bibcode:2007AJ....134.2160R. doi:10.1086/522334.
    2. 1 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 2009-12-27.
    4. ↑ Grundy, W. M. (2004). "Diverse albedos of small trans-neptunian objects". Icarus. 176: 22. arXiv:astro-ph/0502229Freely accessible. 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:0912.3171Freely accessible. Bibcode:2010A&A...511A..72S. doi:10.1051/0004-6361/200913031.
    6. ↑ Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". Retrieved 2006-11-07.
    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/0703098Freely accessible. Bibcode:2007A&A...468L..25P. doi:10.1051/0004-6361:20077294.

    External links


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