  We know that the galactic magnetic field possesses a random component in
addition to the mean uniform component, with comparable strength of the two
components. This random component is considered to play important roles in the
evolution of the interstellar medium (ISM). In this work we present numerical
simulations associated with the interaction of the supersonic flows located at
high latitude in our Galaxy (High Velocity Clouds, HVC) with the magnetized
galactic ISM in order to study the effect that produces a random magnetic field
in the evolution of this objects.
