HII regions and triggered star formation in the turbulent ISM

我们建议详细研究来自大质量恒星的电离辐射对恒星形成的影响，湍流分子云，即如何，以及在什么情况下，大质量恒星可能触发，或加速，然后终止恒星形成。在具有不同统计性质的湍流ISM中，自我维持的、触发的恒星形成可能导致由初始HII区域触发的一颗或多颗大质量恒星的形成，这些恒星将再次引起新的HII区域，并可能引发随后的恒星形成。我们将首次在具有不同初始结构的分子云的高分辨率，三维，重力湍流模拟中深入研究多代HII区域的形成。模拟结果将与斯皮策、赫歇尔和ALMA高空间和光谱分辨率的现有和新的观测结果进行详细比较。为此，我们将采用不同的辐射传输方法来生成连续和线发射图以及光谱能量分布。模拟和地图将通过Astronet恒星形成数据库提供给天体物理学界。

We propose a detailed investigation of the impact of ionizing radiation from massive stars on star-forming, turbulent molecular clouds, i.e. how, and under what circumstances, massive stars may trigger, or accelerate and then terminate star formation. Self-sustained, triggered star formation in a turbulent ISM of different statistical properties may lead to the formation of one or more massive stars triggered by an initial HII region, these stars will again cause new HII regions and may trigger subsequent star formation. For the first time we will thoroughly investigate the formation of multiple generations of HII regions in high-resolution, three-dimensional, gravo-turbulent simulations of molecular clouds with different initial structure. The simulations will be compared in detail to available and new observations with high spatial and spectral resolution with Spitzer, Herschel, and ALMA. For this purpose we will employ different radiative transfer methods to produce continuum and line emission maps as well as spectral energy distributions. The simulations as well as the maps will be made available to the astrophysical community via the Astronet database for star formation.