In this paper, the existence and stability of the out-of-plane equilibrium points of extra-solar planets using the model of the restricted three-body problem, when the central binaries are surrounded by a clusters of material points and their motion is described by the Gylden-Mestschersky problem, is investigated. The masses of the central binaries and the clusters of material points are assumed to vary with time at the same rate in accordance with the unified Mestschersky law. The governing non-autonomous equations of motion of the model is obtained and for a complete transformation to the autonomized systems to be obtainable, we assume that the mass of the clusters of materials varies at the same rate as the masses of the central binaries while the radius and the parameters which determines the density profile of the clusters vary at the same rate as the distances. Thus, we introduce a transformation which defines the mass variation of the clusters with the help of the unified Mestschersky law and the Mestschersky transformation and obtain the autonomized system with constant coefficients. Next, the coordinates of the out-of-plane points are found using perturbation method, the Newton-Raphson's method and analytical approximations in the form of power series in the cluster's mass coefficient. The existence of these points depends solely on the mass variation parameter κ, although the points are however affected by the total mass of the clusters of material points Md and the mass parameter υ. Two pairs of out-of-plane equilibrium points are found; the first pair of equilibrium points L6,7 exists for κ>1 while the second pair L8,9 exists for κ>1 and ξ<υ(κ−1), where ξ is the abscissa of the out-of-plane equilibrium points. Further, for our numerical evidence, we compute the out-of-plane equilibrium points of two extra-solar planets PSR B1620-26b and Kepler-16b, in the binary systems PSR B1620-26 and Kepler-16, respectively. Our numerical results shows that the equilibrium points for PSR B1620-26b, exist when the mass variation parameter and the mass of the clusters lie in the intervals 1<κ≤4 and 0≤Md≤0.04, respectively, while for Kepler-16b, the points exist for 1<κ≤4.1 and 0≤Md≤0.04. Also, it is seen that in the absence of the clusters more out-of-plane equilibrium points evolve and are located far away from the line joining the binaries, while in the presence of the clusters, less out-of-plane equilibrium points evolve, but the evolved points are located closest to the line joining the binaries. Finally, we analyze the stability of the equilibrium points of the autonomized and non-autonomous systems, and both were found to be unstable equilibrium points.