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Uranus Trojans
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Title: Where are the Uranus Trojans?
Authors: Rudolf Dvorak, Ákos Bazsó, Li-Yong Zhou

The area of stable motion for fictitious Trojan asteroids around Uranus' equilateral equilibrium points is investigated with respect to the size of the regions and their shape in dependence of the inclination of the asteroid's orbit. For this task we used the results of extensive numerical integrations of orbits for a grid of initial conditions around the points L4 and L5, and analysed the stability of the individual orbits. Our basic dynamical model was the Outer Solar System (Jupiter, Saturn, Uranus and Neptune). We integrated the equations of motion of fictitious Trojans in the vicinity of the stable equilibrium points up to the age of the Solar system of 5 billion years. One experiment has been undertaken for cuts through the Lagrange points for fixed values of the inclinations, while the semimajor axes were varied. In another run the initial inclination of the asteroids' orbit was varied in the range 0 < i < 60 and the semimajor axes were fixed. It turned out that only four 'windows' of stable orbits survive: these are the orbits for the initial inclinations 0 < i < 7, 9 < i < 13, 31 < i < 36 and 38 < i < 50.

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