  There is considerable observational evidence of implosion of magnetic loop
systems inside solar coronal active regions following high energy events like
solar flares. In this work, we propose that such collapse can be modeled in
three dimensions quite accurately within the framework of ideal
magnetohydrodynamics. We furthermore argue that the dynamics of loop implosion
is only sensitive to the transmitted disturbance of one or more of the system
variables, e.g. velocity generated at the event site. This indicates that to
understand loop implosion, it is sensible to leave the event site out of the
simulated active region. Towards our goal, a velocity pulse is introduced to
model the transmitted disturbance generated at the event site. Magnetic field
lines inside our simulated active region are traced in real time, and it is
demonstrated that the subsequent dynamics of the simulated loops closely
resemble observed imploding loops. Our work highlights the role of plasma
$\beta$ in regards to the rigidity of the loop systems and how that might
affect the imploding loops' dynamics. Compressible magnetohydrodynamic modes
such as kink and sausage are also shown to be generated during such processes,
in accordance with observations.
