  Using 3-dimensional hydrodynamical simulations of isolated dwarf spheroidal
galaxies (dSphs), we undertake an analysis of the chemical properties of their
inner regions, identifying the respective roles played by Type Ia (SNe Ia) and
Type II (SNe II) supernovae. The effect of inhomogeneous pollution from SNe Ia
is shown to be prominent within two core radii, with the stars forming therein
amounting to ~20% of the total. These stars are relatively iron-rich and
alpha-element-depleted compared to the stars forming in the rest of the galaxy.
At odds with the projected stellar velocity dispersion radial profile, the
actual 3-dimensional one shows a depression in the central region, where the
most metal-rich (ie. [Fe/H]-rich) stars are partly segregated. This naturally
results in two different stellar populations, with an anti-correlation between
[Fe/H] and velocity dispersion, in the same sense as that observed in the
Sculptor and Fornax dSphs. Because the most iron-rich stars in our model are
also the most alpha-depleted, a natural prediction and test of our model is
that the same radial segregation effects should exist between [alpha/Fe] and
velocity dispersion.
