  Using a series of three-dimensional, hydrodynamic simulations on an adaptive
grid, we have performed a systematic study on the effect of bubble-induced
motions on metallicity profiles in clusters of galaxies. In particular, we have
studied the dependence on the bubble size and position, the recurrence times of
the bubbles, the way these bubbles are inflated and the underlying cluster
profile. We find that in hydrostatic cluster models, the resulting metal
distribution is very elongated along the direction of the bubbles. Anisotropies
in the cluster or ambient motions are needed if the metal distribution is to be
spherical. In order to parametrise the metal transport by bubbles, we compute
effective diffusion coefficients. The diffusion coefficients inferred from our
simple experiments lie at values of around $\sim 10^{29}$ cm$^2$s$^{-1}$ at a
radius of 10 kpc. The runs modelled on the Perseus cluster yield diffusion
coefficients that agree very well with those inferred from observations.
