The stable region of satellites of large asteroids

Details The stable region of satellites of large asteroids The stable region of satellites of large asteroids

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988icar...75..105z&link_type=abstract

Icarus (ISSN 0019-1035), vol. 75, July 1988, p. 105-112. NSERC-supported research.

Physics

11

Asteroids, Celestial Mechanics, Four Body Problem, Natural Satellites, Dynamic Stability, Eccentric Orbits, Equations Of Motion, Hill Method, Solar Planetary Interactions

Scientific paper

The determination of the stable region of satellites of asteroids is presently addressed through the adoption of the elliptic, planar, restricted four-body problem for the sun-Jupiter-asteroid and satellite system. Numerical experiments conducted on this basis indicate the existence of retrograde satellites almost twice as far from a minor planet as direct satellites; the orbital eccentricity of the minor planet decreases the stable region of its satellite. The results obtained further indicate that Hill's method, while correct for direct motion, is not so for retrograde motion.

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