At the beginning of the Universe, the Big Bang, only light elements such as hydrogen, helium, and lithium are formed. Elements heavier than carbon are formed only in stars and are distributed into the cosmos when the stars die. Among them, so-called alpha elements (O, Mg, Si, S, and Ca) are produced by core-collapse supernova explosions of massive stars, while iron-peak elements are produced predominantly by Type Ia supernovae - thermonuclear explosions of binary star systems. Elements heavier than iron are formed by neutron-capture processes in neutron star mergers and/or magneto-rotational supernovae. Stars are fossils that retain the history of their host galaxies. At the end of their lives, some explode as supernovae, producing heavy elements that are distributed into the interstellar medium. New stars created from this gas contain elements produced by the previous generations of stars. From the spatial distribution of elements, it is therefore possible to constrain the formation and evolutionary histories of the galaxies. This approach, Galactic Archaeology, has been widely used for our Milky Way Galaxy. My team has been running hydrodynamical simulations from cosmological initial conditions including detailed chemical enrichment. First of all, I will show how elemental abundances (from C to U) evolve in a zoom-in simulation of Milky Way-type galaxy, comparing with the observations in the Milky Way. Then I will discuss the origins of the substructures, e.g., the halo, bulge, and thin and thick discs. Finally, I will predict the role of gas infall, outflow, radial flow, and stellar migration in the Milky Way-type galaxy, linking to future observations.