  Recent observations show that the number of stars with very low metallicities
in the dwarf spheroidal satellites of the Milky Way is low, despite the low
average metallicities of stars in these systems. We undertake numerical
simulations of star formation and metal enrichment of dwarf galaxies in order
to verify whether this result can be reproduced with "standard" assumptions.
The answer is likely to be negative, unless some selection bias against very
low metallicity stars is present in the observations.
