The Physics of Star Cluster Formation and Evolution
The Physics of Star Cluster Formation and Evolution
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DOI：
10.1007/s11214-020-00689-4
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发表时间：
2020-05
影响因子：
10.3
通讯作者：
M. Krause;S. Offner;C. Charbonnel;M. Gieles;R. Klessen;E. Vázquez-Semadeni;J. Ballesteros-Paredes;P. Girichidis;J. M. Diederik Kruijssen;J. Ward;H. Zinnecker
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文献类型：
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作者：
M. Krause;S. Offner;C. Charbonnel;M. Gieles;R. Klessen;E. Vázquez-Semadeni;J. Ballesteros-Paredes;P. Girichidis;J. M. Diederik Kruijssen;J. Ward;H. Zinnecker
星星团形成于致密的、分层的塌缩气体云中。大量的动能转化为湍流，恒星由细丝提供的核心形成。在最致密的区域，恒星反馈在去除气体方面效果最差，恒星可能会非常有效地形成。这些区域也是在高质量星团中，来自某种高质量恒星的喷出物在一些低质量恒星的形成阶段被有效地捕获，并被引导到后者形成多个种群。星星团中的星星形成时期通常由气体流动决定，而气体流动决定了星团中气体的丰度。我们认为，有可能只有一个星星形成时代后，集群仍然基本上明确的气体集群风。碰撞动力学在这一阶段是重要的，导致核心崩溃，膨胀和最终分散的每个集群。我们回顾了该领域的最新进展，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 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.