  We investigate effects of a global magnetic field on the dynamics of an
ensemble of clumps within a magnetized advection-dominated accretion flow by
neglecting interactions between the clumps and then solving the collisionless
Boltzman equation. In the strong-coupling limit, in which the averaged radial
and the rotational velocities of the clumps follow the ADAF dynamics, the
averaged radial velocity square of the clumps is calculated analytically for
different magnetic field configurations. The value of the averaged radial
velocity square of the clumps increases with increasing the strength of the
radial or vertical components of the magnetic field. But a purely toroidal
magnetic field geometry leads to a reduction of the value of the averaged
radial velocity square of the clumps at the inner parts with increasing the
strength of this component. Moreover, dynamics of the clumps strongly depends
on the amount of the advected energy so that the value of the averaged radial
velocity square of the clumps increases in the presence of a global magnetic
field as the flow becomes more advective.
