The stability of the planetary triangular Lagrange points
Abstract
From the starting point of the observed existence of Jupiter's two Trojan asteroid families, the question of whether or not stability of motions at their analogous triangular Lagrange points can exist for the other planets is asked. Numerical body integrations of the solar system show significant indications of such stability for the planets from Venus to Neptune. For the terrestrial planets, during a 2 million year integration, stability clearly exist. Near the Lagrangian L4, L5 points the test particles oscillate in tadpole regions. Beyond this the orbits of the particles remain stable but are horseshoe like. In the outer solar system (from Jupiter to Neptune) calculations indicate (at least) 20 million year stability for tadpole like orbits of the Trojans' of various planets. In 20 June 1990 D. H. Levy and H. E. Homlt discovered the asteroid 1990 MB. After orbit calculation E. Bowell suggested that this object may be a Mars' Trojan. This result is now confirmed. A one million year numerical integration of the orbit, based on the orbital elements calculated from observations, indicated stable motion in the neighborhood of Mars' L5 point.
 Publication:

Finnish Physical Society Conference Proceedings
 Pub Date:
 1991
 Bibcode:
 1991fnps.confQV...M
 Keywords:

 Jupiter (Planet);
 Lagrangian Equilibrium Points;
 Planetary Orbits;
 Stability;
 Trojan Orbits;
 Asteroids;
 Digital Simulation;
 Numerical Integration;
 Lunar and Planetary Exploration