Galaxy clusters exhibit a pronounced bimodal distribution in their central properties, split between "Cool Core" (CC) systems with dense, rapidly cooling centers and "Non-Cool Core" (NCC) systems with flat, high-entropy cores. While mergers are thought to disrupt cool cores and transform them into NCCs, simulations struggle to reproduce the observed abundance of NCCs and the resilience of CCs to all but the most major head-on collisions. Furthermore, the "cooling flow problem" persists in CCs, where the predicted massive inflow of cold gas to feed star formation is not observed, implying a tightly regulated AGN feedback loop that is difficult to fine-tune self-consistently over billions of years (Fabian 2012; McDonald et al. 2018).