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We explore the influence of the Milky Way galaxy's chemical evolution on theformation, structure, and habitability of the Solar system. Using a multi-zoneGalactic Chemical Evolution (GCE) model, we successfully reproduce keyobservational constraints, including the age-metallicity ([Fe/H]) relation,metallicity distribution functions, abundance gradients, and [X/Fe] ratiotrends for critical elements involved in planetary mineralogy, including C, O,Mg, and Si. Our GCE model suggests that the Sun formed in the inner Galacticdisc, $R_{\rm birth,\odot}\approx 5$ kpc. We also combined a stoichiometricmodel with the GCE model to examine the temporal evolution and spatialdistribution of planet building blocks (PBBs) within the Milky Way galaxy,revealing trends in the condensed mass fraction ($f_{\rm cond}$),iron-to-silicon mass fraction ($f_{\rm iron}$), and water mass fraction($f_{\rm water}$) over time and towards the inner Galactic disc regions.Specifically, our model predicts a higher $f_{\rm cond}$ in the protoplanetarydisc within the inner regions of the Milky Way galaxy, as well as an increased$f_{\rm iron}$ and a decreased $f_{\rm water}$ in the inner regions. Based onthese findings, we discuss the potential impact of the Sun's birth location onthe overall structure and habitability of the Solar System.

Exploring the Sun's birth radius and the distribution of planet building  blocks in the Milky Way galaxy: A multi-zone Galactic chemical evolution  approach