  The impact of stochastic gas motions on the metal distribution in cluster
core is evaluated. Peaked abundance profiles are a characteristic feature of
clusters with cool cores and abundance peaks are likely associated with the
brightest cluster galaxies (BCGs) which dwell in cluster cores. The width of
the abundance peaks is however significantly broader than the BCG light
distribution, suggesting that some gas motions are transporting metals
originating from within the BCG. Assuming that this process can be treated as
diffusive and using the brightest X-ray cluster A426 (Perseus) as an example,
we estimate that a diffusion coefficient of the order of $2 10^{29} {\rm cm^2
s^{-1}}$ is needed to explain the width of the observed abundance profiles.
Much lower (higher) diffusion coefficients would result in too peaked (too
shallow) profiles. Such diffusion could be produced by stochastic gas motions
and our analysis provides constraints on the product of their characteristic
velocity and their spatial coherence scale. We speculate that the activity of
the supermassive black hole of the BCG is driving the stochastic gas motions in
cluster cores. When combined with the assumption that the dissipation of the
same motions is a key gas heating mechanism, one can estimate both the velocity
and the spatial scale of such a diffusive processes.
