Abstract
Recently, it has been found that a high-velocity gas flow can be formed as results of magnetic activities (magnetic reconnection, magneto-centrifugal force, and so forth) at the upper region of the protoplanetary disk. The gas flow induces shock waves when it interacts with surface of the disk directly. We notice atomic line emissions produced at the shock front. We perform numerical simulations of the propagation of the shock front in order to investigate how the shock front propagates in the disk, how much gas molecules are dissociated, and how much the line luminosity would be produced.
