Signatures of powerful, collimated outflows driven by supermassive black holes are frequently observed in the hot atmospheres of galaxy clusters. The these collimated outflows are stopped by the hot gas and hot, energetic lobes form in the galaxy cluster center. How these lobes interact with their environment, whether they distribute their energy and through wich physical meachanism still is under debate. This project aims to simulate these systems in as much fidelity as possible, including all possible mechanisms and study in detail whether the resulting behaviour matches observations. This way, the exact interaction mechanism can be determined by disproving all alternative scenarios.
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