We set out to constrain the chemical conditions in the early Solar System by analyzing chemical evolution models of protoplanetary disks and comparing them to our current knowledge of Solar System bodies, such as comets. We propose that the region located at 10 AU≤r≤30 AU is ideal for the formation of ice mantles that match observed cometary abundances. The growth of an ice mantle contributes to increase significantly the size of dust grains, which will impact the midplane temperature and the efficiency of dust coagulation.