Stellar Wind Feedback

大质量恒星是决定星系星际介质物理条件的关键因素。在局部范围内，它们通过强烈的辐射、强风和超新星爆炸迅速摧毁恒星形成的分子云。超新星反馈似乎是银河系尺度上的三种机制中占主导地位的，但早期的前SN反馈似乎是负责破坏纳塔尔分子云和限制质量最大的恒星。恒星风反馈的重要性仍然不确定。最近的工作表明，在热冲击恒星风和周围物质之间的界面处的湍流混合可能会强烈冷却热气体，限制这种反馈机制的强度。您将使用3D流体动力学模拟研究此过程。您的计算将使用最先进的代码，并利用利兹大学和其他地方的高性能计算设施。您将能够对湍流混合的重要性和恒星风反馈的有效性施加新的约束。

Massive stars are key agents in setting the physical conditions in the interstellar medium in galaxies. On local scales, they rapidly destroy star-forming molecular clouds through their intense radiation, powerful winds, and supernova explosions. Supernova feedback seems to be the dominant of the three mechanisms on galactic scales, but early, pre-SN feedback appears to be responsible for destroying the natal molecular cloud and in limiting the mass of the most massive stars. The importance of stellar wind feedback is still uncertain. Recent work has shown that turbulent mixing at the interface between the hot shocked stellar wind and surrounding material may strongly cool the hot gas, limiting the strength of this feedback mechanism. You will investigate this process using 3D hydrodynamical simulations. Your calculations will use a state-of-the-art code and make use of high-performance computing facilities at The University of Leeds and potentially elsewhere. You will be able to place new constraints on the importance of turbulent mixing and the effectiveness of stellar wind feedback.