  A three dimensional Smoothed Particle Hydrodynamical (SPH) model has been
extended to study the radiative driven implosion effect of massive stars on the
dynamical evolutions of surrounding molecular clouds. The new elements in the
upgraded code are the inclusion of Lyman continuum in the incident radiation
flux and the treatment of hydrogen ionisation process; introducing ionisation
heating & recombination cooling effects; and adding a proper description of the
magnetic and turbulent pressures to the internal pressure of the molecular
cloud. The application of this newly developed model to the structure of the
middle Eagle Nebula finger suggests that the shock induced by the ionising
radiation at the front side of the head precedes an ionisation front moving
towards the center of the core, and that the core at the fingertip is at
transition stage evolving toward a state of induced star formation. The
dynamical evolution of the velocity field of the simulated cloud structure is
discussed to illustrate the role of the self-gravity and the different cloud
morphologies which appear at different stages in the evolutionary process of
the cloud. The modelled gas evaporation rate is consistent with that of current
other models and the density, temperature and chemical profiles are agreement
with the observed values. The relative lifetimes of different simulated cloud
morphologies suggests a possible answer to the question of why more
bright-rimmed clouds are observed to possess a flat-core than an elongated-core
morphology. [Abridged]
