Many problems in coronal physics can be treated to first order as problems reducable to MHD. Examples include the propogation and dissipation of MHD waves, magnetic reconnection and flux emergence into the corona. Many of these problems require complex geometries in order to capture the important physics. This combined with non-linearities makes the problem compuational in nature. Currently computational techniques are being use to solve problems on wave leakage from staight and curved flux tubes, flare excitation of loop oscillations, emergence of flux tubes through the photosphere/chromospheric layers and the dynamics magnetic reconnection.