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There is considerable observational evidence of implosion of magnetic loopsystems inside solar coronal active regions following high energy events likesolar flares. In this work, we propose that such collapse can be modeled inthree dimensions quite accurately within the framework of idealmagnetohydrodynamics. We furthermore argue that the dynamics of loop implosionis only sensitive to the transmitted disturbance of one or more of the systemvariables, e.g. velocity generated at the event site. This indicates that tounderstand loop implosion, it is sensible to leave the event site out of thesimulated active region. Towards our goal, a velocity pulse is introduced tomodel the transmitted disturbance generated at the event site. Magnetic fieldlines inside our simulated active region are traced in real time, and it isdemonstrated that the subsequent dynamics of the simulated loops closelyresemble observed imploding loops. Our work highlights the role of plasma$\beta$ in regards to the rigidity of the loop systems and how that mightaffect the imploding loops' dynamics. Compressible magnetohydrodynamic modessuch as kink and sausage are also shown to be generated during such processes,in accordance with observations.

Simulating coronal loop implosion and compressible wave modes in a flare hit active region