  The case of the planar circular photogravitational restricted three-body
problem where the more massive primary is an emitter of radiation is
numerically investigated. A thorough numerical analysis takes place in the
configuration $(x,y)$ and the $(x,C)$ space in which we classify initial
conditions of orbits into three main categories: (i) bounded, (ii) escaping and
(iii) collisional. Our results reveal that the radiation pressure factor has a
huge impact on the character of orbits. Interpreting the collisional motion as
leaking in the phase space we related our results to both chaotic scattering
and the theory of leaking Hamiltonian systems. We successfully located the
escape as well as the collisional basins and we managed to correlate them with
the corresponding escape and collision times. We hope our contribution to be
useful for a further understanding of the escape and collision properties of
motion in this interesting version of the restricted three-body problem.
