  We present results for the chemical evolution of the Galactic bulge in the
context of an inside-out formation model of the Galaxy. A supernova-driven wind
was also included in analogy with elliptical galaxies. New observations of
chemical abundance ratios and metallicity distribution have been employed in
order to check the model results. We confirm previous findings that the bulge
formed on a very short timescale with a quite high star formation efficiency
and an initial mass function more skewed toward high masses than the one
suitable for the solar neighbourhood. A certain amount of primary nitrogen from
massive stars might be required to reproduce the nitrogen data at low and
intermediate metallicities.
