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Previous work based on non-radiative cosmological hydrodynamical simulations have defined the shock radius, $r_\\text{shock}$, using the ICM entropy, $K \\propto T/{n_\\mathrm{e}}^{2/3}$, where $T$ and $n_\\text{e}$ are the ICM temperature and electron density respectively; the $r_\\text{shock}$ is identified with either the radius at which $K$ is a maximum or at which its logarithmic slope is a minimum. 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Sullivan, C. Power, K. Walker, M. Zhang, W. Cui, X. Zhang, Y. Li","submitted_at":"2024-12-13T05:07:50Z","abstract_excerpt":"Observations of the intracluster medium (ICM) in the outskirts of galaxy clusters reveal shocks associated with gas accretion from the cosmic web. Previous work based on non-radiative cosmological hydrodynamical simulations have defined the shock radius, $r_\\text{shock}$, using the ICM entropy, $K \\propto T/{n_\\mathrm{e}}^{2/3}$, where $T$ and $n_\\text{e}$ are the ICM temperature and electron density respectively; the $r_\\text{shock}$ is identified with either the radius at which $K$ is a maximum or at which its logarithmic slope is a minimum. 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