The chemical evolution of asymptotic giant branch (AGB) stars depends greatly on the input physics (e.g., mass loss recipe, convective model). Variations in the hot bottom burning (HBB) strength, third dredge-up (TDU) efficiency and AGB evolutionary timescale are among the main consequences of adopting different input physics. The ATON evolutionary code stands apart from others in that it uses the Blöcker mass loss prescription and the Full Spectrum of Turbulence (FST) convective model. We have developed an s-process module for ATON by extending the element network from 30 to 320 elements, which uses the physical inputs (such as temperature or density) calculated by ATON. Here we present the first preliminary results of s-process nucleosynthesis for ATON AGB models with different progenitor masses. These preliminary results are compared with predictions from other AGB nucleosynthesis models that use different input physics. We also outline our future tasks to improve the current s-process ATON simulations.