2011 QF99
| Discovery | |
|---|---|
| Discovery date | 2011[1] |
| Designations | |
| centaur | |
| Orbital characteristics[2][1] | |
| Epoch 13 January 2016 (JD 2457400.5) | |
| Uncertainty parameter 3 | |
| Observation arc | 1449 days (3.97 yr) |
| Aphelion | 22.487 AU (3.3640 Tm) |
| Perihelion | 15.676 AU (2.3451 Tm) |
| 19.081 AU (2.8545 Tm) | |
| Eccentricity | 0.17846 |
| 83.35 yr (30445 d) | |
| 277.47° | |
| Inclination | 10.8233° |
| 222.5096° | |
| 287.63° | |
| Earth MOID | 14.7043 AU (2.19973 Tm) |
| Jupiter MOID | 10.4391 AU (1.56167 Tm) |
| Physical characteristics | |
| Dimensions | ~60 km[2] |
| 0.05 (assumed) | |
| 9.6 (r-band)[2] 9.7[1] |
|
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2011 QF99 is the first and, as of 2015, the only known Uranus trojan.[2][3] It was discovered in 2011 during a deep survey of trans-Neptunian objects conducted with the Canada–France–Hawaii Telescope.[2][4] It is believed to be roughly 60 km in diameter, assuming an albedo of 0.05.[2]
2011 QF99 temporarily orbits near Uranus's L4 Lagrangian point (leading Uranus). It will continue to librate around L4 for at least 70,000 years and will remain a Uranus co-orbital for up to three million years before becoming a centaur. 2011 QF99 is thus a temporary Uranus trojan—a centaur captured some time ago.[2]
Uranus trojans are generally expected to be unstable and none of them are thought to be of primordial origin. A simulation led to the conclusion that at any given time, 0.4% of the centaurs in the scattered population within 34 AU would be Uranus co-orbitals, of which 64% (0.256% of all centaurs) would be in horseshoe orbits, 10% (0.04%) would be quasi-satellites, and 26% (0.104%) would be trojans (evenly split between the L4 and L5 groups).[2]
References
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<references />, or <references group="..." />External links
- 2011 QF99 at the JPL Small-Body Database
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