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Orbital stability of high inclination asteroids

Published online by Cambridge University Press:  25 May 2016

N. A. Solovaya  and
E. M. Pittich
N. A. Solovaya
Affiliation:
Celestial Mechanics Department Sternberg State Astronomical Institute University Prospect 13, 119 889 Moscow, Russia
E. M. Pittich
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences Dúbravská cesta 9, 842 28 Bratislava, Slovak Republic

Abstract

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The orbital evolutions of fictitious asteroids with high inclinations have been investigated. The selected initial orbits represent asteroids with movement, which corresponds to the conditions of the Tisserand invariant for C = C (L1) in the restricted three body problem. Initial eccentricities of the orbits cover the interval 0.0–0.4, inclinations the interval 40–80°, and arguments of perihelion the interval 0–360°. The equations of motion of the asteroids were numerically integrated from the epoch March 25, 1991 forward within the interval of 20,000 years, using a dynamical model of the solar system consisting of all planets. The orbits of the model asteroids are stable at least during the investigated period.

Type
Part IV - Asteroids: Theory and Ephemerides
Information
Symposium - International Astronomical Union , Volume 172: Dynamics, Ephemerides and Astrometry of the Solar System , 1996 , pp. 187 - 192
Copyright
Copyright © Kluwer 1996 

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