Abstract We couple a simplified model for galactic chemical evolution with software that models the condensation of dust in protoplanetary disks and software that models the interior structure of planets, in order to estimate the effects that galactic chemical evolution has on the properties of planets as they form over time. We find that the early abundances of elements formed from the evolution and death of high-mass stars (such as oxygen, silicon, and magnesium) yields planets with larger mantles and smaller cores. The later addition of elements produced in low-mass stars (such as iron and nickel) causes the planet cores to become relatively larger. The result is planets that orbit older stars are less dense than planets orbiting younger stars. These results are broadly consistent with recent observations of planet properties from stars of varying ages.