  We revisit the problem of the flat slope of the Mg2 versus <Fe> relationship
found for nuclei of elliptical galaxies (Faber et al. 1992; Worthey et al.
1992; Carollo et al. 1993; Davies et al. 1993), indicating that the Mg/Fe ratio
should increase with galactic luminosity and mass. We transform the abundance
of Fe, as predicted by classic wind models and alternative models for the
chemical evolution of elliptical galaxies, into the metallicity indices Mg2 and
<Fe>, by means of the more recent index calibrations and show that none of the
current models for the chemical evolution of elliptical galaxies is able to
reproduce exactly the observed slope of the <Fe> versus Mg2 relation, although
the existing spread in the data makes this comparison quite difficult. In other
words, we can not clearly discriminate between models predicting a decrease
(classic wind model) or an increase of such a ratio with galactic mass. The
reason for this resides in the fact that the available observations show a
large spread due mostly to the errors in the derivation of the <Fe> index. In
our opinion this fact prevents us from drawing any firm conclusion on the
behaviour of Mg and Fe in these galaxies.
