  We present a 2-dimensional chemical evolution code applied to a Milky Way
type galaxy, incorporating the role of spiral arms in shaping azimuthal
abundance variations, and confront the predicted behaviour with recent
observations taken with integral field units. To the usual radial distribution
of mass, we add the surface density of the spiral wave and study its effect on
star formation and elemental abundances. We compute five different models: one
with azimuthal symmetry which depends only on radius, while the other four are
subjected to the effect of a spiral density wave. At early times, the imprint
of the spiral density wave is carried by both the stellar and star formation
surface densities; conversely, the elemental abundance pattern is less
affected. At later epochs, however, differences among the models are diluted,
becoming almost indistinguishable given current observational uncertainties. At
the present time, the largest differences appear in the star formation rate
and/or in the outer disc (R$\ge$ 18\,kpc). The predicted azimuthal oxygen
abundance patterns for $t \le 2$\,Gyr are in reasonable agreement with recent
observations obtained with VLT/MUSE for NGC 6754
