The problem studied in this paper models the system of four bodies, three of which are of finite mass (primaries), moving in elliptic orbits around the centre of mass always maintaining the configuration of Lagrange’s triangular solution. That is the primaries are always at the vertices of an equilateral triangle. The fourth body is of infinitesimal mass and therefore does not affect the movement of the primaries. We will discuss the effect on the dynamics of the problem when the largest primary is a luminous body while the other two are oblate spheroids of similar mass. We have used simulation techniques to demonstrate how different parameters such as mass ratio, radiation pressure of the largest primary, oblateness of the two equal mass primaries, and eccentricity of the orbits traced by the primaries influence the number and existence of equilibrium points. The pulsating surfaces of zero velocity of the elliptic triangular restricted four body problem are studied. The projection of the zero velocity surfaces on xy− and xz−planes are also studied along with the low-velocity sub-regions in the xy−plane. The linear stability of the equilibrium points was also studied numerically.