  Flare associated coronal shock waves sometimes interact with solar
prominences leading to large amplitude prominence oscillations. Such prominence
activation gives us unique opportunity to track time evolution of shock-cloud
interaction in cosmic plasmas. Although the dynamics of interstellar
shock-cloud interaction is extensively studied, coronal shock-solar prominence
interaction is rarely studied in the context of shock-cloud interaction.
Associated with X5.4 class solar flare occurred on 7 March, 2012, a globally
propagated coronal shock wave interacted with a polar prominence leading to
large amplitude prominence oscillation. In this paper, we studied bulk
acceleration and excitation of internal flow of the shocked prominence using
three-dimensional MHD simulations. We studied eight magnetohydrodynamic (MHD)
simulation runs with different mass density structure of the prominence, and
one hydrodynamic simulation run, and compared the result. In order to compare
observed motion of activated prominence with corresponding simulation, we also
studied prominence activation by injection of triangular shaped coronal shock.
We found that magnetic tension force mainly accelerate (and then decelerate)
the prominence. The internal flow, on the other hand, is excited during the
shock front sweeps through the the prominence and damps almost exponentially.
We construct phenomenological model of bulk momentum transfer from shock to the
prominence, which agreed quantitatively with all the simulation results. Based
on the phenomenological prominence-activation model, we diagnosed physical
parameters of coronal shock wave. The estimated energy of the coronal shock is
several percent of total energy released during the X5.4 flare.
