Abstract
Against the background of a restricted three-body problem consisting of a supergiant eclipsing binary system, the two primaries are composed of a pair of bright oblate stars whose mass changes with time. The zero-velocity surface and curve of the problem are numerically studied to describe the third body’s motion area, and the corresponding five libration points are obtained. Moreover, the effect of small perturbations, Coriolis and centrifugal forces, radiative pressure, and the oblateness and mass parameters of the two primaries on the third body’s dynamic behavior is discussed through the bifurcation diagram. Furthermore, the second- and third-order approximate analytical periodic solutions around the collinear solution point L3 in two-dimensional plane and three-dimensional spaces are presented by using the Lindstedt-Poincaré perturbation method.
Highlights
It is well known that Newton’s famous proposition “Principle” took a decisive step in our understanding of the universe
In the theoretical framework of scalar-tensor gravitation, Zhou et al [4] found that there is a collinear solution to the three-body problem in the presence of a scalar field, and studied the effect of the scalar field on this solution and the positions of Lagrange points through numerical examples
The three-body problem is widely used in the evolution of binary systems [6] and the dynamic analysis of binary asteroids [7,8], as well as other fields in the universe such as dark matter, galaxies, GW170817 (GW is short for gravitational wave), and Mukhanov-Sasaki Hamiltonian dynamics, and so forth
Summary
It is well known that Newton’s famous proposition “Principle” took a decisive step in our understanding of the universe. Based on the model of the binary system proposed in Reference [39], Gao and Wang [6] continued to study the analytical approximate periodic solutions around the collinear libration points They examined the influence of the small perturbation in Coriolis and centrifugal forces, the triaxiality, and radiation pressure of the primaries on the third body’s dynamic behavior through the bifurcation diagram. The effects of small perturbations, Coriolis and centrifugal forces, radiation pressure, and the oblateness and variable mass of the primaries on the third body’s dynamic behavior will be discussed numerically through bifurcation diagram in the context of an R3BP consisting of a supergiant eclipsing binary system.
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
