Fig. 14.
Evolution of the [M/H] (left panel) and [α/Fe] (right panel) abundance ratios of our best-fit models computed at 4, 8, and 12 kpc compared with the abundances observed in a stellar sample in the solar annulus (Silva Aguirre et al. 2018). Magenta points depict the high-α population, whereas green points indicate the low-α one. As in Spitoni et al. (2019a, 2020), we have not taken into account young α-rich stars.
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