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Galaxy cluster outskirts mark the transition region from the mildlynon-linear cosmic web to the highly non-linear, virialised, cluster interior.It is in this transition region that the intra-cluster medium (ICM) begins toinfluence the properties of accreting galaxies and groups, as ram pressureimpacts a galaxy's cold gas content and subsequent star formation rate.Conversely, the thermodynamical properties of the ICM in this transition regionshould also feel the influence of accreting substructure (i.e. galaxies andgroups), whose passage can drive shocks. In this paper, we use a suite ofcosmological hydrodynamical zoom simulations of a single galaxy cluster, drawnfrom the nIFTy comparison project, to study how the dynamics of substructureaccreted from the cosmic web influences the thermodynamical properties of theICM in the cluster's outskirts. We demonstrate how features evident in radialprofiles of the ICM (e.g. gas density and temperature) can be linked to strongshocks, transient and short-lived in nature, driven by the passage ofsubstructure. The range of astrophysical codes and galaxy formation models inour comparison are broadly consistent in their predictions (e.g. agreeing whenand where shocks occur, but differing in how strong shocks will be); this is aswe would expect of a process driven by large-scale gravitational dynamics andstrong, inefficiently radiating, shocks. This suggests that mapping such shockstructures in the ICM in a cluster's outskirts (via e.g. radio synchrotronemission) could provide a complementary measure of its recent merger andaccretion history.

nIFTy Galaxy Cluster simulations VI: The dynamical imprint of substructure on gaseous cluster outskirts