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In order to understand the roles of metal flows in galaxy formation andevolution, we analyse our self-consistent cosmological chemo-dynamicalsimulation of a Milky Way like galaxy during its thin-disc phase. Our simulatedgalaxy disc qualitatively reproduces the variation of the dichotomy in[$\alpha$/Fe]-[Fe/H] at different Galactocentric distances as derived byAPOGEE-DR16, as well as the stellar age distribution in [$\alpha$/Fe]-[Fe/H]from APOKASC-2. The disc grows from the inside out, with a radial gradient inthe star-formation rate during the entire phase. Despite the radial dependence,the outflow-to-infall ratio of metals in our simulated halo shows atime-independent profile scaling with the disc growth. The simulated discundergoes two modes of gas inflow: (i) an infall of metal-poor and relativelylow-[$\alpha$/Fe] gas, and (ii) a radial flow where already chemically-enrichedgas moves inwards with an average velocity of $\sim0.7$ km/s. Moreover, we findthat stellar migrations mostly happen outwards, on typical time scales of$\sim5$ Gyr. Our predicted radial metallicity gradients agree with theobservations from APOGEE-DR16, and the main effect of stellar migrations is toflatten the radial metallicity profiles by 0.05 dex/kpc in the slopes. We alsoshow that the effect of migrations can appear more important in [$\alpha$/Fe]than in the [Fe/H]-age relation of thin-disc stars.

Stellar migrations and metal flows -- Chemical evolution of the thin disc of a simulated Milky Way analogous galaxy