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From the chemo-dynamical properties of tidal debris in the Milky Way, it hasbeen inferred that the dwarf satellites that have been disrupted had differentchemical abundances from their present-day counterparts of similar mass thatsurvive today, specifically, they had lower [Fe/H] and higher [Mg/Fe]. Here weuse the ARTEMIS simulations to study the relation between the chemicalabundances of disrupted progenitors of MW-mass galaxies and their stellar mass,and the evolution of the stellar mass - metallicity relations (MZR) of thispopulation with redshift. We find that these relations have significantscatter, which correlates with the accretion redshifts ($z_{\rm acc}$) ofsatellites, and with their cold gas fractions. We investigate the MZRs of dwarfpopulations accreted at different redshifts and find that they have similarslopes, and also similar with the slope of the MZR of the surviving population($\approx 0.32$). However, the entire population of disrupted dwarfs displays asteeper MZR, with a slope of $\approx 0.48$, which can be explained by thechanges in the mass spectrum of accreted dwarf galaxies with redshift. We findstrong relations between the (mass-weighted) $\langle z_{\rm acc} \rangle$ ofthe disrupted populations and their global chemical abundances($\langle$[Fe/H]$\rangle$ and $\langle$[Mg/Fe]$\rangle$), which suggests thatchemical diagnostics of disrupted dwarfs can be used to infer the types ofmerger histories of their hosts. For the case of the MW, our simulationspredict that the bulk of the disrupted population was accreted at $\langlez_{\rm acc} \rangle \approx 2$, in agreement with other findings. We also findthat disrupted satellites form and evolve in denser environments, closer totheir hosts, than their present-day counterparts.

Differences in the properties of disrupted and surviving satellites of Milky-Way-mass galaxies in relation to their host accretion histories