  Studies of filamentary structures that are prevalent throughout the
interstellar medium are of great significance to a number of astrophysical
fields. Here, we present 3D hydrodynamic simulations of shock-filament
interactions where the equation of state has been softened to become almost
isothermal. We investigate the effect of such an isothermal regime on the
interaction (where both the shock and filament are isothermal), and we examine
how the nature of the interaction changes when the orientation of the filament,
the shock Mach number, and the filament density contrast are varied. We find
that only sideways-oriented filaments with a density contrast of $10^2$ form a
three-rolled structure, dissimilar to the results of a previous study.
Moreover, the angle of orientation of the filament plays a large role in the
evolution of the filament morphology: the greater the angle of orientation, the
longer and less turbulent the wake. Turbulent stripping of filament material
leading to fragmentation of the core occurs in most filaments; however,
filaments orientated at an angle of $85^{\circ}$ to the shock front do not
fragment and are longer-lived. In addition, values of the drag time are
influenced by the filament length, with longer filaments being accelerated
faster than shorter ones. Furthermore, filaments in an isothermal regime
exhibit faster acceleration than those struck by an adiabatic shock. Finally,
we find that the drag and mixing times of the filament increase as the angle of
orientation of the filament is increased.
