  We investigate the metallicity effect (measured by the original 22Ne content)
on the detailed nucleosynthetic yields for 3D hydrodynamical simulations of the
thermonuclear burning phase in SNe Ia. Calculations are based on post-processes
of the ejecta, using passively advected tracer particles, as explained in
details by Travaglio et al.(2004). The nuclear reaction network employed in
computing the explosive nucleosynthesis contains 383 nuclear species. For this
work we use the high resolution multi-point ignition (bubbles) model b30_3d_768
(Travaglio et al.2004 for the solar metallicity case), and we cover a
metallicity range between 0.1xZ_sun up to 3xZ_sun. We find a linear dependence
of the 56Ni mass ejected on the progenitor's metallicity, with a variation in
the 56Ni mass of ~25% in the metallicity range explored. Moreover, the largest
variation in 56Ni occurs at metallicity greater than solar. Almost no
variations are shown in the unburned material 12C and 16O. The largest
metallicity effect is seen in the alpha-elements. Finally, implications for the
observed scatter in the peak luminosities of SNe Ia are also discussed.
