Chemical evolution in planet-forming regions with growing grains

[Abridged] Planets and their atmospheres are built from gas solid material in protoplanetary disks. This grows smaller, micron-sized grains to larger sizes the disks, during process of planet formation. Our goal is model compositional evolution volatile ices on different sizes, assuming both time-dependent grain growth several constant sizes. The state-of-the-art Walsh chemical kinetics code utilised for modeling evolution. has been upgraded account time-evolving solids. Chemical modelled locally at four radii a disk midplane up 10Myr. five one where size changes with time according appropriate midplane. Local growth, conservation total mass assumption spherical grains, acts reduced grain-surface area that available ice-phase reactions. reduces these reactions efficiency compared scenario conventional grain-size choice 0.1$\mu$m. leads increased abundances H$_{2}$O ice. For carbon inner disk, CO overtake CO$_{2}$ ice as dominant carrier, outer CH$_{4}$ become carrier. Overall, adopted almost identical evolution, when evolving A choice, albeit than 0.1$\mu$m, may therefore be an simplification approximating impact