Simulations of galaxy winds and their interaction with the hot intracluster medium

In modern theories of galaxy formation and evolution, star formation within a galaxy is shut down by two different mechanisms: 1) outflows of gas caused by direct energy injection from exploding supernova and/or jets expelled from supermassive black holes and 2) removal of gas caused by the interaction of galaxies with hot gas contained within groups and clusters. However, our understanding of how these processes work in isolation is woefully incomplete and their interaction is even more poorly understood. It is the goal of this project to understand how these two mechanisms work together to quench the star formation in galaxies. In the first stage of this project, we will run magnetic hydrodynamic (MHD) simulations of gas outflows within isolated galaxies to quantify the effect magnetic fields have on the outflow and reincorporation rates of supernova-driven gas. Secondly, we will model the interaction of these galaxy-wide winds with the hot, magnetized, X-ray emitting plasma of galaxy groups and clusters. Ultimately, these results will have important implications for our understanding of the growth of stellar mass within galaxies and of magnetic fields on galaxy formation.