Massive Star Feedback and Triggered Star Formation: Confronting multi-wavelength observations of the Carina Nebula with numerical simulations

船底座星云是距离我们最近的区域（D=2.3 kpc），拥有大量的大质量恒星（> 65颗O型恒星），是研究剧烈的大质量星星形成以及大质量星星反馈效应的理想场所，这些反馈通过恒星风、电离辐射和膨胀的超级气泡对周围环境产生影响。我们目前正在对船底座恒星形成复合体进行全面的多波长（X射线，红外线和亚毫米）观测，以研究年轻恒星与其分子环境的相互作用。结合现有的HST，Spitzer，MSX和其他数据集，这些数据将使我们能够揭示年轻恒星和原恒星的完整种群，并研究它们的年龄，质量函数，空间分布和盘属性，并确定复杂的冷分子云和热气体的形态，运动学和化学。我们将使用我们新开发的并行光滑粒子流体动力学代码（IVINE），可以有效地处理来自大质量年轻恒星的电离辐射对湍流气体环境的影响，这些数据与数值模拟进行详细的比较。这是第一次，我们将包括恒星风与恒星紫外辐射电离的分子气体。这将使我们能够获得对基本过程的新的和详细的见解，例如大质量恒星对分子云的破坏，分子云和HII区域之间界面处观察到的复杂柱状结构的起源，恒星反馈对分子云动力学和湍流的影响，电离辐射和恒星风如何触发第二代恒星的形成，以及原恒星盘如何在这样的环境中形成和演化。

As the most nearby (D=2.3 kpc) southern region with a large population of massive stars (> 65 O-type stars), the Carina Nebula is an ideal site to study violent high-mass star formation and the effects of massive star feedback, via stellar winds, ionizing radiation, and expanding superbubbles, on their surroundings. We are currently performing comprehensive multi-wavelength (X-ray, infrared, & sub-mm) observations of the Carina star-forming complex to study the interaction of the young stars with their molecular environment. In combination with existing HST, Spitzer, MSX, and other data sets, these data will allow us to reveal the complete populations of young stars and protostars and to study their ages, mass functions, spatial distributions and disk properties, and determine the morphology, kinematics, and chemistry of cold molecular clouds and the hot gas in the complex. We will perform a detailed comparison of these data with numerical simulations using our newly developed parallel Smooth Particle Hydrodynamics code (IVINE) that allows an efficient treatment of the effect of ionizing radiation from massive young stars on the turbulent gaseous environment. For the first time, we will include stellar winds in combination with the stellar UV radiative ionization of the molecular gas. This should allow us to obtain new and detailed insights into fundamental processes such as the disruption of molecular clouds by massive stars, the origin of the observed complex pillar-like structures at the interfaces between molecular clouds and HII regions, the effect of stellar feedback on molecular cloud dynamics and turbulence, how ionising radiation and the stellar winds trigger the formation of a second generation of stars and how protostellar disks form and evolve in such an environment.