Uranus Trojans are asteroids that coexist with Uranus in its orbit around the Sun. Initially predicted through simulations, astronomers have confirmed the existence of two such trojans, which both are located at Uranus’s Lagrangian point L4, leading the planet in its path. The first, (687170) 2011 QF99, was classified as a Uranus Trojan in 2013 and followed by (636872) 2014 YX49, which was identified as the second in 2017.
Several theories attempt to explain how these Trojans came to orbit Uranus. The most widely accepted hypothesis, gravitational scattering, suggests that these asteroids or comets were gravitationally influenced by other planets, guiding them either directly into Uranus’s orbit or into regions where Uranus's gravitational pull remains balanced.[1]
| Designation | Cloud | Semi-major Axis | Perihelion | Eccentricity | Inclination | Absolute Magnitude | Diameter |
|---|---|---|---|---|---|---|---|
| 2011 QF99 | L4 | 19.167 | 15.765 | 0.177 | 10.796 | 9.6 | 60 |
| 2014 YX49 | L4 | 19.113 | 13.762 | 0.279 | 25.524 | 8.79 | 77 |
Gallery[]
References[]
- ↑ Uranus trojans - Wikipedia
| Small Solar System Bodies including comets | ||
|---|---|---|
| Cis-Neptunian | NEO | ꞌAylóꞌchaxnim • Atrias • Apollos • Arjunas • Amors • Venus Trojan • Earth Trojans • Mars Trojans • Quasi-Satellites |
| Main Belt/Jupiter Trojans | Asteroids • Various Collisional Families • Ceres/Vesta Trojans • Hilda • Jupiter Trojans • Quasi-Satellites | |
| Distant/Centaur | Centaur • Damocloid • Saturn Trojan • Uranus Trojans • Neptune Trojans | |
| TNO | Kuiper Belt/KBO | Classical (Cold • Hot) • Resonant (Plutino • Twotino) |
| Scattered disc/SDO | Resonant | |
| ETNO | ESDO | |
| EDDO | Sednoid → Oort Cloud Objects | |
| Comets | NEC • Sungrazing/Kreutz Sungrazing • Remnant • Extinct • Lost • Jupiter • Quasi-Hilda • Halley-type | |