![]() Animation of 2011 QF99 relative to Sun and Uranus 1600-2500 2011 QF99 · Uranus · Sun | |
Discovery | |
---|---|
Discovered by | M. Alexandersen[1] |
Discovery site | Mauna Kea Obs. |
Discovery date | 29 August 2011[2] (first observation only) |
Designations | |
2011 QF99 | |
Uranus trojan[3] centaur[2] · distant[1] | |
Orbital characteristics[2] | |
Epoch 4 September 2017 (JD 2458000.5) | |
Uncertainty parameter 3 | |
Observation arc | 3.97 yr (1,449 days) |
Aphelion | 22.422AU |
Perihelion | 15.659 AU |
19.040 AU | |
Eccentricity | 0.1776 |
83.08yr (30,346 days) | |
283.84° | |
0° 0m 42.84s / day | |
Inclination | 10.833° |
222.52° | |
288.25° | |
Physical characteristics | |
60 km(calculated)[3] | |
0.05(assumed)[3] | |
9.6(R-band)[3] 9.7[2] | |
(687170) 2011 QF99 is aminor planet from theouter Solar System and the first knownUranus trojan to be discovered. It measures approximately 60 kilometers (37 miles) in diameter, assuming an albedo of 0.05.[3][4] It was first observed 29 August 2011 during a deep survey of trans-Neptunian objects conducted with theCanada–France–Hawaii Telescope, but its identification as Uranian trojan was not announced until 2013.[3][5]
2011 QF99 temporarily orbits near Uranus'sL4Lagrangian point (leading Uranus). It will continue tolibrate around L4 for at least 70,000 years and will remain a Uranusco-orbital for up to three million years.2011 QF99 is thus a temporary Uranus trojan—a centaur captured some time ago.[3][6]
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 inhorseshoe orbits, 10% (0.04%) would bequasi-satellites, and 26% (0.104%) would be trojans (evenly split between the L4 and L5 groups).[3] A second Uranian Trojan,2014 YX49, was announced in 2017.[7]