报告题目：How to Make Massive Stars: the First Steps
报 告 人：王科 博士（欧南台博士后）
报告人简介：Dr. Ke Wang is a postdoctoral fellow at the European Southern Observatory (ESO) with functional work at the European ALMA (Atacama Large Millimeter/submillimeter Array) Regional Center. He received his Ph.D. from Peking University in 2012. Majority of his Ph.D. program was carried out at the Harvard-Smithsonian Center for Astrophysics during a predoctoral fellowship with duty at the Submillimeter Array (SMA), the only submillimeter interferometer before ALMA. He was then awarded a European Union grant to conduct his first postdoc at the Kapteyn Astronomical Institute in the Netherlands. Afterwards, he joined ESO in 2012. He is an enthusiastic observer with expertise in radio interferometers, a frequent user of SMA and the Jansky Very Large Array (VLA), now an ALMA astronomer on duty. His main research interest is the early phase of massive star formation, from Planck cold cores, infrared dark clouds to interstellar filaments.
报告摘要：Massive stars drive the evolution of galaxies, but how they come into existence is still a fundamental open question. Particularly critical and poorly understood is the very early stage, which determines how initial conditions in molecular clouds lead to the onset of star formation. In this talk, I will present our series studies on infrared dark clouds (IRDCs) aiming to characterize the early stage. Seen as shadows against the Galactic IR background, IRDCs are extremely cold and dense molecular clouds that represent the early stage in massive star formation. Our dedicated observing campaign is carefully designed to resolve the initial fragmentation and at the time to measure the gas temperature and turbulence. This coordinated effort allows us to infer the nature of the fragmentation and to constrain theoretical models. We find that the early stage is characterized by hierarchical fragmentation of IRDCs. The fragmentation at multiple levels leads to structures at multiple spatial scales, ranging from ~1 pc down to ~0.01 pc, where turbulence dominates the fragmentation at all the probed scales. The results are yet to be fully implemented by theoretical models. If time permits, I will also introduce my functional work at ALMA (Atacama Large Millimeter/submillimeter Array), the next generation radio interferometry.
报告时间：4月23日（周三）上午11:00
报告地点：（北京西路2号）紫台大楼619会议室
联 系 人：徐瑾瑜（83332000）
欢迎各位老师、同学参加！
