Abstract
This paper explores the motion of an infinitesimal body around the triangular equilibrium points in the framework of circular restricted three-body problem (CR3BP) with the postulation that the primaries are triaxial rigid bodies, radiating in nature and are also under the influence of Poynting–Robertson (P-R) drag. We study the linear stability of these triangular points and for the numerical application, the binary stars Kruger 60 (AB) and Archird have been considered. These triangular points are not only perceived to move towards the line joining the primaries in the direction of the bigger primary with increasing triaxiality, they are also unstable owing to the destabilizing influence of P-R drag.
Highlights
The restricted three-body problem (R3BP) describes profoundly, the motion of three masses in space whose initial positions, velocities and acceleration are known from which their future motion can be predicted
The masses are such that they have a common gravitational attraction with the two massive bodies influencing the motion of the third body, while the later has an insignificant effect on the primaries. This R3BP constitutes one of the most recognized problems in dynamical astronomy because the exploits that have been witnessed in attempt to understand and explain the dynamics of the R3BP has allowed great historical, theoretical, practical and educational thrive by mankind
Examination of the R3BP has been a subject of interest to researchers for over two hundred years and has had significant impact in numerous scientific fields including, among others, celestial mechanics, chaos theory, galactic dynamics and molecular physics
Summary
The restricted three-body problem (R3BP) describes profoundly, the motion of three masses in space whose initial positions, velocities and acceleration are known from which their future motion can be predicted. The motion of the test particle in the vicinity of two radiating bodies, having PR-drags was examined by [34] and they established numerically the positions of the triangular equilibrium points lying outside the orbital plane. These points are seen to be unstable due to the presence of PR-drags. For the case were the smaller primary is an emitter of radiation having PR-drag, with a bigger oblate body, [25] showed numerically using exact values and approximations that the triangular points exist but are unstable due to the destabilizing effect of PR-drag.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
