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 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.

中文翻译：

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星团形成与演化的物理学

星团形成于密集、分层坍塌的气体云中。大量动能转化为湍流，恒星由细丝供给的核心形成。在最致密的区域，恒星反馈在去除气体方面最不有效，恒星可能非常有效地形成。在这些区域，在大质量星团中，某些大质量恒星的喷射物在一些低质量恒星的形成阶段被有效捕获，并被引导到后者形成多个星族。星团中的恒星形成时期通常由决定星团中气体丰度的气体流动决定。我们认为可能只有一个恒星形成时期之后，星团在星团风的作用下基本上保持无气体。碰撞动力学在导致核心坍塌的这个阶段很重要，每个集群的扩展和最终分散。我们回顾了该领域的最新发展，重点是理论工作。