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Radio relics are arc-like synchrotron sources at the periphery of galaxyclusters, produced by cosmic-ray electrons in a $\mu$G magnetic field which arebelieved to have been (re-)accelerated by merger shock fronts. However, not allrelics appear at the same location as shocks as seen in the X-ray. In aprevious work, we suggested that the shape of some relics may result from thepre-existing spatial distribution of cosmic-ray electrons, and tested thishypothesis using simulations by launching AGN jets into a cluster atmospherewith sloshing gas motions generated by a previous merger event. We showed thatthese motions could transport the cosmic ray-enriched material of the AGNbubbles to large radii and stretch it in a tangential direction, producing afilamentary shape resembling a radio relic. In this work, we improve ourphysical description for the cosmic rays by modeling them as a separate fluidwhich undergoes diffusion and Alfv\'en losses. We find that including thisadditional cosmic ray physics significantly diminishes the appearance of thesefilamentary features, showing that our original hypothesis is sensitive to themodeling of cosmic ray physics in the intracluster medium.

Turning AGN bubbles into radio relics with sloshing: modeling CR transport with realistic physics