  In this work we have assumed a Hernquist model with an inside-out formation
for the Galactic bulge and, using a chemical evolution model, we were able
obtain the bulge metallicity distribution function (MDF) for different radial
regions. The preliminary results show that in the inner regions of the bulge
the MDF has a higher fraction of metal poor stars, while this fraction is
progressively diminished as moving outwards in the bulge. These results may
explain the metallicity gradient observed in the Galactic bulge.
