论文标题
星团形成和进化的物理
The Physics of Star Cluster Formation and Evolution
论文作者
论文摘要
恒星簇形成密集的，分层崩溃的气云。散装动能转化为湍流，由细丝喂养的核心形成的恒星。在最紧凑的区域中，恒星反馈在去除气体和恒星中的有效性最小，可能会非常有效地形成。这些区域也是在高质量簇中，在某些低质量恒星的形成阶段有效地捕获了某种高质量恒星的射出，并有效地引入了后者以形成多个种群。恒星簇中的恒星形成时期通常是由确定簇中气体丰度的气流设置的。我们认为，可能只有一个恒星形成时期，之后簇基本上仍然清除了簇风的气体。在此阶段，碰撞动力学很重要，从而导致核心崩溃，扩展和最终分散每个集群。我们回顾了该领域的最新发展，重点是理论工作。
Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.
