 Hubble Space Telescope image of 1996 TO66 taken in 2005 | |
| Discovery | |
|---|---|
| Discovered by | |
| Discovery date | 12 October 1996 |
| Designations | |
| (19308) 1996 TO66 | |
| |
| 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 (103,555 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 | |
| 7.92 h (0.330 d) | |
| 7.92 h[2] | |
| 0.7 (assumed) | |
| Temperature | ~43 K |
| 4.5 | |
(19308) 1996 TO66 (provisional designation 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
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
- ^ a b 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. S2CID 8387493.
- ^ a b "JPL Small-Body Database Browser: 19308 (1996 TO66)" (2003-10-18 last obs). Retrieved 5 April 2016.
- ^ 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.
- ^ Grundy, W. M. (2004). "Diverse albedos of small trans-neptunian objects". Icarus. 176 (1): 184–191. arXiv:astro-ph/0502229. Bibcode:2005Icar..176..184G. doi:10.1016/j.icarus.2005.01.007. S2CID 118866288.
- ^ Snodgrass, Carry; Dumas, Hainaut (16 December 2009). "Characterisation of candidate members of (136108) Haumea's family". Astronomy and Astrophysics. 511: A72. arXiv:0912.3171. Bibcode:2010A&A...511A..72S. doi:10.1051/0004-6361/200913031.
- ^ 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.
- ^ 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. S2CID 18546361.
External links
- First Rotation Period of a Kuiper Belt Object Measured – ESO, 5 November 1998
- (19308) 1996 TO66 at the JPL Small-Body Database
| Moons and rings |  | |
|---|---|---|
| Classification | ||
| Collisional family | ||
| Controversy | ||
 | This article about a centaur (minor planet) or trans-Neptunian object is a stub. You can help Wikipedia by expanding it. |
This page was last edited on 18 January 2024, at 20:49