Abstract
In a synodic-pulsating dimensionless coordinate, with a luminous primary and an oblate secondary, we examine the effects of radiation pressure, oblateness (quadruple and octupolar i.e. ) and eccentricity of the orbits of the primaries on the triangular points in the ER3BP. have been shown to disturb the motion of an infinitesimal body and particularly has significant effects on a satellite’s secular perturbation and orbital precessions. The influence of these parameters on the triangular points of Zeta Cygni, 54 Piscium and Procyon A/B are highlighted in this study. Triangular points are stable in the range and their stability is affected by said parameters.
Highlights
“Small bodies” play a special and important role in the spectrum of exploration of matter in both the solar and stellar systems
The motion of the infinitesimal body when at least one of the participating bodies is an intense emitter of radiation called the photogravitational circular R3BP (CR3BP) was formulated by Radzievsky (1950)
Taking account of the oblateness of the earth, Ammar et al (2102) have conducted an analytic theory of the motion of a satellite and solved the equations of the secular variations in a closed form, while Abouelmagd (2012) analyzed the effect of oblateness of the more massive primary up to J4 in the planar CR3BP and proved that the positions and stability of the triangular points are affected by this perturbation
Summary
“Small bodies” (comets, asteroids, satellites and dust particles) play a special and important role in the spectrum of exploration of matter in both the solar and stellar systems. The photogravitational restricted three-body problem models adequately the motion of a particle of a gas-dust cloud which is in the field of two gravitating and radiating stars. JJ4 has significant effects in the satellite’s secular perturbation and orbital precessions These shifts are quite relevant in a number of practical applications including global gravity field determination (Konopliv et al 2013 and Renzetti 2013) and fundamental physics in space Iorio 2005, 2006, 2007a, b; Singh and Umar 2013c, & Umar and Singh 2014, 2015). Taking account of the oblateness of the earth, Ammar et al (2102) have conducted an analytic theory of the motion of a satellite and solved the equations of the secular variations in a closed form, while Abouelmagd (2012) analyzed the effect of oblateness of the more massive primary up to J4 in the planar CR3BP and proved that the positions and stability of the triangular points are affected by this perturbation.
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