2023MNRAS.526.6088B

We explore the influence of the Milky Way galaxy's chemical evolution on the formation, structure, and habitability of the Solar system. Using a multizone Galactic chemical evolution (GCE) model, we successfully reproduce key observational constraints, including the age-metallicity ([Fe/H]) relation, metallicity distribution functions, abundance gradients, and [X/Fe] ratio trends for critical elements involved in planetary mineralogy, including C, O, Mg, and Si. Our GCE model suggests that the Sun formed in the inner Galactic disc, R_birth,⊙ ≈ 5 kpc. We also combined a stoichiometric model with the GCE model to examine the temporal evolution and spatial distribution of planet building blocks within the Milky Way galaxy, revealing trends in the condensed mass fraction (f_cond), iron-to-silicon mass fraction (f_iron), and water mass fraction (f_water) over time and towards the inner Galactic disc regions. Specifically, our model predicts a higher f_cond in the protoplanetary disc within the inner regions of the Milky Way galaxy, as well as an increased f_iron and a decreased f_water in the inner regions. Based on these findings, we discuss the potential impact of the Sun's birth location on the overall structure and habitability of the Solar system.