The impact of radiation pressure and from massive stars on the turbulent interstellar medium in extreme environments

对于极端环境中高度湍流的星际介质，如富含气体的高红移盘和相互作用的星系，辐射压力-星际气体/尘埃对星光的吸收-被认为是云分裂的主要原因，可能是观测到的大尺度星系风的主要发射机制。拟议的项目旨在通过数值模拟了解这一基本的风力驱动过程，其来源是无法通过直接观测获得的母体巨型分子云。我们计划系统地研究大质量短寿命恒星通过电离和辐射压力输入的能量对湍流ISM的影响，并将使用高分辨率三维模拟-包括重力、流体动力学和辐射传输-来自嵌入湍流分子云中的大质量恒星的反馈，包括首次对星光与星际气体/尘埃的耦合和由此产生的动量输入的自洽模拟。这一反馈过程对恒星形成效率、云寿命、湍流和风力驱动的影响将被研究。

For the highly turbulent interstellar medium in extreme environments, like gas-rich high-redshift disks and interacting galaxies, radiation pressure - the absorption of starlight by interstellar gas/dust – is supposed to dominate cloud disruption and can be the main launching mechanism of observed large scale galactic winds. The proposed project is aimed at understanding this fundamental wind driving process with numerical simulations at its origin, the parental giant molecular cloud which is not accessible by direct observations. We propose to systematically investigate the impact of energy input from massive short-lived stars by ionization and radiation pressure on the turbulent ISM and will use high-resolution three-dimensional simulations - including gravity, hydrodynamics, and radiation transfer - of the feedback from massive stars embedded in turbulent molecular clouds including, for the first time, a self-consistent modeling of the coupling of starlight to the interstellar gas/dust and the resulting momentum input. The effect of this feedback process on the star formation efficiency, cloud lifetimes, turbulence, and wind driving will be investigated.