  The X-ray emission by hot gas around the central galaxies of galaxy clusters
is commonly modeled assuming the existence of steady-state, multiphase cooling
flows. The inflowing gas will be chemically enriched by type Ia supernovae and
stellar mass loss occurring in the outer parts of the central galaxy. This may
give rise to a substantial metallicity enhancement towards the center, whose
amplitude is proportional to the ratio of the central galaxy luminosity to the
mass inflow rate. The metallicity of the hotter phases is expected to be higher
than that of the colder, denser phases. The metallicity profile expected for
the Centaurus cluster is in good agreement with the iron abundance gradient
recently inferred from ASCA measurements (Fukazawa et al. 1994). However,
current data do not rule out alternative models where cooling is balanced by
some heat source. In either case, the enhancement expected from injection by
type Ia supernovae is roughly as observed. Most of this work is described in
more detail in Reisenegger, Miralda-Escud\'e, \& Waxman (1996;
astro-ph/9511044).
