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

在现代星系形成和演化理论中，星系内的恒星形成是由两种不同的机制关闭的：1)由爆炸超新星的直接能量注入和/或超大质量黑洞喷出的射流引起的气体流出，2)由星系与群和星团内的热气体相互作用引起的气体移除。然而，可悲的是，我们对这些过程是如何孤立地工作的理解是不完整的，对它们之间的相互作用更是知之甚少。这个项目的目标是了解这两种机制是如何共同作用来抑制星系中恒星的形成。在该项目的第一阶段，我们将对孤立星系内的气体流出进行磁流体动力学（MHD）模拟，以量化磁场对超新星驱动气体流出和再合并率的影响。其次，我们将模拟这些星系范围内的风与星系群和星系团的热的、磁化的、发射x射线的等离子体的相互作用。最终，这些结果将对我们理解星系内恒星质量的增长以及磁场对星系形成的影响具有重要意义。

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.