A method based on considerations of the tidal disruption force produced by the gravitational field of the Galaxy is applied to the determination of the distances of high-velocity H I clouds and the Magellanic stream. The shapes of the small-scale condensations observed within the clouds are used as indicators of tidal disruption forces, allowing the estimation of the upper or lower limits of the galactocentric distance at which the condensations are stable against the tidal disruption force. A lower limit to the distance of the condensations making up complex A of 14 kpc from the sun is obtained under the assumption of free-fall-like kinematics. The northern portion of the Magellanic Stream is estimated to be less than about 50 kpc from the galactic center, as are the H I clouds apparently associated with the Sculptor galaxies NGC 55 and NGC 300. Finally, the very high velocity H I clouds observed in the southern sky are also estimated to have distances similar to that of the Magellanic Stream, although some appear to have distances greater than 90 kpc.