The systematic motion of the interstellar clouds at the galactic shock region

The galactic rotation curve for the interstellar clouds is calculated, considering the dynamical interactions between the clouds and the intercloud medium which produced the galactic shock waves. We consider the dynamical interactions due to the turbulent viscosity of the intercloud medium and due to the bow shock waves produced ahead the clouds. It is shown that the rotation curve for the clouds becomes more smooth than that for the intercloud medium, and that the difference between the rotation curve for the clouds and the observed rotation curve is considerably reduced. (auth.)