  Elliptical galaxies are often assumed to be the primary source of heavy
elements in the intracluster medium (ICM), with the contribution of other
morphological types being negligible. In this paper we argue that a role of
spiral galaxies in the chemical evolution of the ICM is also important. This
statement rests upon our recent calculations of the heavy element loss from a
disk galaxy through the hot steady-state galactic wind and dust grains
expulsion by stellar radiation pressure. We show that a typical disk galaxy is
nearly as effective in enriching the ICM as an elliptical galaxy of the same
mass. Having estimated the oxygen and iron loss from a single galaxy, we
integrate them over the galactic mass spectrum. We show that the "effective"
loss (per unit luminosity) from spiral galaxies is comparable to the loss from
ellipticals. The dominant role of early-type galaxies in rich clusters is
caused by that they outnumber spirals.
