Hostname: page-component-78c5997874-lj6df Total loading time: 0 Render date: 2024-11-14T23:18:04.759Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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 

References

Abalakin, V.K. (1989) Astronomicheskij Ezhegodnik na 1991 god. Nauka, Leningrad.Google Scholar
Everhart, E. (1985) An efficient integrator that used Gauss-Radau spacing, Dynamics of Comets: Their Origin and Evolution, (Carusi, A. and Valsecchi, G. B., Eds.), pp. 185–202, Reidel, Dordrecht.Google Scholar
Gerasimov, I.A. and Solovaya, N.A. (1989) Evolution of the resonant group of minor planets of the outer part of the asteroidal belt, Asteroids Comets Meteors III, (Lagerkvist, C.-I., Rickman, H., Linblad, B.A., and Lindgren, M., Eds.), pp. 91–94, Uppsala University, Uppsala.Google Scholar
Kozai, Y. (1962) Secular perturbations of asteroids with high inclination and eccentricity, Astronomical Journal, Vol. no. 67, pp. 591–598.Google Scholar
Solovaya, N.A., Gerasimov, I.A., and Pittich, E.M. (1992) 3-D Orbital Evolution Model of Outer Asteroid Belt, Asteroids, Comets, Meteors 1991, (Harris, A.W. and Bowell, E., Eds.), pp. 565–568, Lunar and Planetary Institute, Houston, Texas.Google Scholar