High-velocity clouds are flows of neutral hydrogen, located at high galactic latitudes, with large velocities ([VLSR]≥ 100 km/s) that do not match a simple model of circular rotation for our Galaxy. Numerical simulations have been performed for the last 20 years to study the details of their evolution, and their possible interaction with the Galactic disk. Here we present a brief review of the models that have been already published, and describe newly performed three-dimensional magnetohydrodynamic simulations.