  From the chemo-dynamical properties of tidal debris in the Milky Way, it has
been inferred that the dwarf satellites that have been disrupted had different
chemical abundances from their present-day counterparts of similar mass that
survive today, specifically, they had lower [Fe/H] and higher [Mg/Fe]. Here we
use the ARTEMIS simulations to study the relation between the chemical
abundances of disrupted progenitors of MW-mass galaxies and their stellar mass,
and the evolution of the stellar mass - metallicity relations (MZR) of this
population with redshift. We find that these relations have significant
scatter, which correlates with the accretion redshifts ($z_{\rm acc}$) of
satellites, and with their cold gas fractions. We investigate the MZRs of dwarf
populations accreted at different redshifts and find that they have similar
slopes, and also similar with the slope of the MZR of the surviving population
($\approx 0.32$). However, the entire population of disrupted dwarfs displays a
steeper MZR, with a slope of $\approx 0.48$, which can be explained by the
changes in the mass spectrum of accreted dwarf galaxies with redshift. We find
strong relations between the (mass-weighted) $\langle z_{\rm acc} \rangle$ of
the disrupted populations and their global chemical abundances
($\langle$[Fe/H]$\rangle$ and $\langle$[Mg/Fe]$\rangle$), which suggests that
chemical diagnostics of disrupted dwarfs can be used to infer the types of
merger histories of their hosts. For the case of the MW, our simulations
predict that the bulk of the disrupted population was accreted at $\langle
z_{\rm acc} \rangle \approx 2$, in agreement with other findings. We also find
that disrupted satellites form and evolve in denser environments, closer to
their hosts, than their present-day counterparts.
