| To study the galactic chemical abundances and their evolution through numerical simulations, we have worked on an update of the GADGET3 code. This version incorporates chemical enrichment by SNII, SNIa, and AGB stars, and utilizes the KROME chemical package to model the formation of molecular hydrogen (H2) and improve the representation of thermal and radiative processes. A DTD scheme is employed for SNIa, allowing for the reproduction and study of abundance ratios of different elements with respect to iron, as obtained from observations. Additionally, the enrichment by AGB stars contributes to the carbon (C) abundance which plays a role in our models as a non-equilibrium cooling precursor. By consistently obtaining the H2 content at runtime, we have incorporated into the star formation model, a dependence on the H2 fraction which is in turn influenced by a developed model of the local stellar radiation field and its attenuation. Evaluations have been performed to understand the impact of physical parameters and prescriptions, leading to improved agreement between the chemical properties of the simulated systems and observations of galaxies with significant star formation. A good agreement also has been found with the Kennicutt-Schmidt molecular law, indicating a more realistic representation of star formation. The next step is to study these behaviors during simulations of galactic interactions, where metallicity profiles and the star formation rate have been analyzed. |
