Abstract In the present work, we employ the modified elliptic restricted three-body problem by considering some additional perturbed forces such as: the radiation pressure, the primaries’ oblateness, and the effect of dust belt for studying the dynamical motion of the infinitesimal body. The semi-analytical solutions for the locations of non-collinear equilibrium points are obtained. The proposed model is applied to real astronomical systems. Thus, the Sun–Mars and the Proxima Centauri systems are used to estimate numerically and graphically the locations of these points in both systems at different values of perturbation parameters. In this context, the critical mass values are evaluated for both systems to analyze the stability motion of the infinitesimal body around the locations of equilibrium points and find the stability range of these locations. We demonstrate that the stability of non-collinear points in both systems depends on the parameter of mass ratio values of its own system. It is observed that the locations of these points and their stability will be affected significantly due to the changes in the values of perturbation parameters.
Highlights The perturbed elliptical restricted three-body problem. The semi-analytical solutions for the locations of non-collinear equilibrium points. The locations of non-collinear equilibrium points for Sun–Mars and Proxima Centauri systems. The estimation of critical mass values for Sun–Mars and Proxima Centauri systems. The stability analysis of the infinitesimal body motion around the locations of non-collinear equilibrium points.
Analysis of stability of non-collinear equilibrium points: Application to Sun–Mars and Proxima Centauri systems
Acta Astronautica ; 204 ; 199-206
2022-12-22
8 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
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