  The aim of this work is to compare the orbital dynamics in three different
models describing the properties of a star cluster rotating around its parent
galaxy in a circular orbit. In particular, we use the isochrone and the
Hernquist potentials to model the spherically symmetric star cluster and we
compare our results with the corresponding ones of a previous work in which the
Plummer model was applied for the same purpose. Our analysis takes place both
in the configuration $(x,y)$ and in the phase $(x,\dot{x})$ space in order to
elucidate the escape process as well as the overall orbital properties of the
tidally limited star cluster. We restrict our investigation into two dimensions
and we conduct a thorough numerical analysis distinguishing between ordered and
chaotic orbits as well as between trapped and escaping orbits, considering only
unbounded motion for several energy levels above the critical escape energy. It
is of particular interest to determine the escape basins towards the two exit
channels (near the Lagrangian points $L_1$ and $L_2$) and relate them with the
corresponding escape times of the orbits.
