  Individual abundances in the Milky Way disc record stellar birth properties
(e.g. age, birth radius ($R_{\rm birth}$)) and capture the diversity of the
star-forming environments over time. Assuming an analytical relationship
between ([Fe/H], [$\alpha$/Fe]) and $R_{\rm birth}$, we examine the
distributions of individual abundances [X/Fe] of elements C, O, Mg, Si, Ca
($\alpha$), Al (odd-z), Mn (iron-peak), Y, and Ba (neutron-capture) for stars
in the Milky Way. We want to understand how these elements might differentiate
environments across the disc. We assign tracks of $R_{\rm birth}$ in the
[$\alpha$/Fe] vs. [Fe/H] plane as informed by expectations from simulations for
$\sim 59,000$ GALAH stars in the solar neighborhood ($R\sim7-9$ kpc) which also
have inferred ages. Our formalism for $R_{\rm birth}$ shows that older stars
($\sim$10 Gyrs) have a $R_{\rm birth}$ distribution with smaller mean values
(i.e., $\bar{R}_{\mbox{birth}}$$\sim5\pm0.8$ kpc) compared to younger stars
($\sim6$ Gyrs; $\bar{R}_{\mbox{birth}}$$\sim10\pm1.5$ kpc), for a given [Fe/H],
consistent with inside-out growth. The $\alpha$-, odd-z, and iron-peak element
abundances decrease as a function of $R_{\rm birth}$, whereas the
neutron-capture abundances increase. The $R_{\rm birth}$-[Fe/H] gradient we
measure is steeper compared to the present-day gradient (-0.067 dex/kpc vs
-0.058 dex/kpc), which we also find true for $R_{\rm birth}$-[X/Fe] gradients.
These results (i) showcase the feasibility of relating the birth radius of
stars to their element abundances, (ii) the abundance gradients across $R_{\rm
birth}$ are steeper than those over current radius, and (iii) offer an
observational comparison to expectations on element abundance distributions
from hydrodynamical simulations.
