Heavy element evolution in the inner regions of the Milky Way
  We present results for the evolution of the abundances of heavy elements (O,
Mg, Al, Si, K, Ca, Cr, Mn, Ni and Fe) in the inner Galactic regions ($R_{GC} <
4$kpc). We adopt a detailed chemical evolution model already tested for the
Galactic bulge and compare the results with APOGEE data. We start with a set of
yields from the literature which are considered the best to reproduce the
abundance patterns in the solar vicinity. We find that in general the predicted
trends nicely reproduce the data but in some cases either the trend or the
absolute values of the predicted abundances need to be corrected, even by large
factors, in order to reach the best agreement. We suggest how the current
stellar yields should be modified to reproduce the data and we discuss whether
such corrections are reasonable in the light of the current knowledge of
stellar nucleosynthesis. However, we also critically discuss the observations.
Our results suggest that Si, Ca, Cr and Ni are the elements for which the
required corrections are the smallest, while for Mg and Al moderate
modifications are necessary. On the other hand, O and K need the largest
corrections to reproduce the observed patterns, a conclusion already reached
for solar vicinity abundance patterns, with the exception of oxygen. For Mn we
apply corrections already suggested in previous works. \end{abstract}
