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Trojan (celestial body)

In astronomy, a trojan is a small celestial body (mostly asteroids) that shares the orbit of a larger body, remaining in a stable orbit approximately 60° ahead of or behind the main body near one of its Lagrangian points L4 and L5. Trojans can share the orbits of planets or of large moons.

Trojan minor planets
are seen in this graphic as Greek camp at ahead of Jupiter and as Trojan camp at trailing Jupiter along its orbital path. It also shows the asteroid belt between Mars and Jupiter and the Hilda asteroids. In 1772, the Italian–French mathematician and astronomer Joseph-Louis Lagrange obtained two constant-pattern solutions (collinear and equilateral) of the general three-body problem. In the restricted three-body problem, with one mass negligible (which Lagrange did not consider), the five possible positions of that mass are now termed Lagrange points. On February 12th, 1906, Max Wolf discovered the trojan asteroid 588 Achilles; His contemporary Carl Charlier noticed that the asteroid was caught in the point of Jupiter, and thus 588 Achilles was the first discovered instance of Lagrange's theoretical calculations applying in practice. The term "trojan" originally referred to the "trojan asteroids" (Jovian trojans) that orbit close to the Lagrangian points of Jupiter. These have long been named for figures from the Trojan War of Greek mythology. By convention, the asteroids orbiting near the point of Jupiter are named for the characters from the Greek side of the war, whereas those orbiting near the of Jupiter are from the Trojan side. There are two exceptions, named before the convention was adopted: 624 Hektor in the L4 group, and 617 Patroclus in the L5 group. Astronomers estimate that the Jovian trojans are about as numerous as the asteroids of the asteroid belt. Later on, objects were found orbiting near the Lagrangian points of Neptune, Mars, Earth, Uranus, and Venus. Minor planets at the Lagrangian points of planets other than Jupiter may be called Lagrangian minor planets. • Four Martian trojans are known: 5261 Eureka, , , and – the only Trojan body in the leading "cloud" at , There seem to be, also, , , and , but these have not yet been accepted by the Minor Planet Center. • There are 28 known Neptunian trojans, but the large Neptunian trojans are expected to outnumber the large Jovian trojans by an order of magnitude. • was confirmed to be the first known Earth trojan in 2011. It is located in the Lagrangian point, which lies ahead of the Earth. was found to be another Earth trojan in 2021. It is also at L4. • was identified as the first Uranus trojan in 2013. It is located at the Lagrangian point. A second one, , was announced in 2017. • Saturn has 1 known trojan in the L4 Lagrangian Point, 2019 UO14. Trojans by planet ==Stability==
Stability
Whether or not a system of star, planet, and trojan is stable depends on how large the perturbations are to which it is subject. If, for example, the planet is the mass of Earth, and there is also a Jupiter-mass object orbiting that star, the trojan's orbit would be much less stable than if the second planet had the mass of Pluto. As a rule of thumb, the system is likely to be long-lived if m1 > 100m2 > 10,000m3 (in which m1, m2, and m3 are the masses of the star, planet, and trojan). More formally, in a three-body system with circular orbits, the stability condition is 27(m1m2 + m2m3 + m3m1) 1 + m2 + m3)2. So the trojan being a mote of dust, m3→0, imposes a lower bound on of ≈ 24.9599. And if the star were hyper-massive, m1→+∞, then under Newtonian gravity, the system is stable whatever the planet and trojan masses. And if = , then both must exceed 13+√168 ≈ 25.9615. However, this all assumes a three-body system; once other bodies are introduced, even if distant and small, stability of the system requires even larger ratios. ==See also==
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