The abundances of the heavy elements beyond iron that we observe today in the solar system are mainly the result of the two nucleosynthesis processes: the slow neutron capture (s-) process and the rapid neutron capture (r-) process. Low-mass Asymptotic Giant Branch (AGB) (2 < M /M ⊙ < 3) and massive (M /M ⊙ > 10) stars have been identified as the sites of the s-process. We provide a new set of low-mass AGB models with initial masses M /M ⊙ = 2,3 and Z = 0.01, 0.02 and 0.03. Internal gravity wave mixing is the physics mechanism responsible for the formation of a 13 C-pocket on average three times larger than our previous data set. Consequently the s-process production is significantly enhanced. Abundances are compared to other stellar datasets available in the literature and to a wide range of observations, including carbon-stars, barium stars, post-AGB stars, and pre-solar grains. The full nucleosynthesis was calculated in post-processing using the NuGrid mppnp code.