  We develop a model for the metal enrichment of the intracluster medium (ICM)
that combines a cosmological non-radiative hydrodynamical N-Body/SPH simulation
of a cluster of galaxies, and a semi-analytic model of galaxy formation. The
novel feature of our hybrid model is that the chemical properties of the
diffuse gas in the underlying simulation are dynamically and consistently
generated from stars in the galaxies. We follow the production of several
chemical elements, provided by low- and intermediate-mass stars, core collapse
and type Ia supernovae. We analyse the spatial distribution of metals in the
ICM, investigate the way in which the chemical enrichment proceeds, and use
iron emissivity as a tracer of gas motions. Fe and O radial abundance profiles
are enhanced in the inner 100 h^-1 kpc in the last Gyr because of the
convergence of enriched gas clumps to the cluster centre. Our results support a
scenario in which part of the central intracluster gas comes from gas clumps
that, in the redshift range of z~0.2 to ~0.5, have been enriched to solar
values and are at large distances from the cluster centre (from ~1 to ~6 h^-1
Mpc) moving at very high velocities (from ~1300 to ~2500 km s^-1). The
turbulent gas motions within the cluster, originated in the inhomogeneous gas
infall during the cluster assembly, are manifested in emission-weighted
velocity maps as gradients that can be as large as ~1000 km s^-1 over distances
of a few hundred kpc. Gradients of this magnitude are also seen in velocity
distributions along sightlines through the cluster centre. Doppler shifting and
broadening suffered by the Fe K 6.7 keV emission line along such sightlines
could be used to probe these gas large-scale motions when they are produced
within an area characterised by high iron line emissivity.
