  We study the s-process abundances at the epoch of the Solar-system formation
as the outcome of nucleosynthesis occurring in AGB stars of various masses and
metallicities. The calculations have been performed with the Galactic chemical
evolution (GCE) model presented by Travaglio et al. (1999, 2004). With respect
to previous works, we used updated solar meteoritic abundances, a neutron
capture cross section network that includes the most recent measurements, and
we implemented the $s$-process yields with an extended range of AGB initial
masses. The new set of AGB yields includes a new evaluation of the 22Ne(alpha,
n)25Mg rate, which takes into account the most recent experimental information.
