In this paper, we examine the stability of the equilibrium points in the photogravitational circular restricted fourbody problem by considering all the masses are varying with time, one of the three masses are taken as source of radiation pressure and all the masses are placed at the vertices of an equilateral triangle. We derive the equations of motion under the effect of solar radiation pressure by using the Meshcherskii transformations. We have plotted the equilibrium points, time series, surfaces of motion of infinitesimal body, Poincare surface of sections and NewtonRaphson basin of attraction. Here five equilibrium points are found but it is ten in the classical case. From the time series, it is observed that the orbit will not be periodic. The surfaces of motion of the infinitesimal body are studied in the space. The Poincare surface of section is in the discrete type of pattern. The convergence of the equilibrium points is studied by the NewtonRaphson basin of attraction. Finally, we have examined the stability of the equilibrium points and found that all the equilibrium points are unstable.
Key words: Radiation Pressure; variable masses; equilateral triangle; Poincare surface of sections; NewtonRaphson basin of attraction.
