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 hight 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.