Feedback in Young Stellar Clusters

目前的恒星形成理论可以很好地描述孤立的年轻低质量恒星的形成和演化，但很难解释大质量恒星的起源--这些恒星是在具有各种能量反馈过程的星团环境中形成的。这项研究项目的目标是通过观测大质量原恒星形成和演化的早期阶段，建立一个大质量恒星形成的经验理论。这将需要分析来自(亚)毫米和厘米波长射电望远镜的高分辨率数据，特别是阿塔卡马大毫米/亚毫米阵列、亚毫米阵列和扬斯基甚大阵列。射频数据将使观测高度嵌入的年轻大质量原恒星成为可能。连续发射和线发射都将被用来追踪原星系团中的气体分布和运动学，从而深入了解大质量恒星形成过程中涉及的各种物理过程，包括质量吸积和外流。观测结果将与大质量恒星和星团形成的数值模型的模拟观测结果进行比较。

Current theories of star formation can describe the formation and evolution of isolated, young low-mass stars well, but struggle to explain the origin of massive stars- forming in clustered environments with a variety of energetic feedback processes. The goal of this research project is to build an empirical theory of massive star formation by observing massive protostars in the early stages of their formation and evolution. This will require analysing high-resolution data from (sub)mm and cm-wavelength radio telescopes, in particular the Atacama Large Millimeter/sub-millimeter Array (ALMA), the Submillimeter Array (SMA) and the Jansky Very Large Array (VLA). The radio frequency data will make the observation of young highly-embedded massive protostars possible. Both continuum and line emission will be used to trace the gas distribution and kinematics in protoclusters, providing an insight to the various physical processes involved in massive star formation, including mass accretion and outflows. The observational results will be compared with simulated observations of numerical models of massive star and cluster formation.