Motion in the generalized restricted three-body problem

This paper investigates the motion of an infinitesimal body in the generalized restricted three-body problem. It is generalized in the sense that both primaries are radiating, oblate bodies, together with the effect of gravitational potential from a belt. It derives equations of the motion, locates positions of the equilibrium points and examines their linear stability. It has been found that, in addition to the usual five equilibrium points, there appear two new collinear points L (n1), L (n2) due to the potential from the belt, and in the presence of all these perturbations, the equilibrium points L (1), L (3) come nearer to the primaries; while L (2), L (4), L (5), L (n1) move towards the less massive primary and L (n2) moves away from it. The collinear equilibrium points remain unstable, while the triangular points are stable for 0