用宏观探索微观：从星团系统的性质到星团形成区的性质
Probing the Microscopic with the Macroscopic: from Properties of Star Cluster Systems to Properties of Cluster-Forming Regions
摘要：
了解星团系统是如何达到它们目前观测到的性质的，是对团簇形成物理学的一个强有力的探索，而不需要求助于遥远星系中单个团簇形成区（CFRg）的高空间分辨率观测。在这篇文章中，我专注于CFRgs的质量-半径关系，如何通过研究形成星团的气体排出阶段来揭示它，以及它的含义是什么。我证明，通过潮汐场暴露的星团的影响，CFRg质量半径关系规则集群婴儿的重量损失依赖于集群质量。观测约束的时不变斜率的幂律年轻的集群质量函数是鲁棒满足CFRgs具有恒定的平均体积密度。相反，一个恒定的平均表面密度将有利于优先销毁高质量的集群。因此，一个纯粹的动力学推理导致了一个与恒星形成一致的结论，这是一个由体积密度阈值驱动的过程。进一步发展这一概念，分子团和CFRgs的性质自然会分离。这允许理解：（i）为什么星团质量函数比分子云（团）质量函数陡峭;（ii）在分子结构的质量尺寸空间中存在大质量恒星形成极限。
英文摘要：
To understand how systems of star clusters have reached their presently observed properties constitutes a powerful probe into the physics of cluster formation, without needing to resort to high spatial resolution observations of individual cluster-forming regions (CFRg) in distant galaxies. In this contribution I focus on the mass-radius relation of CFRgs, how it can be uncovered by studying the gas expulsion phase of forming star clusters, and what the implications are. I demonstrate that, through the tidal field impact upon exposed star clusters, the CFRg mass-radius relation rules cluster infant weight-loss in dependence of cluster mass. The observational constraint of a time-invariant slope for the power-law young cluster mass function is robustly satisfied by CFRgs with a constant mean volume density. In contrast, a constant mean surface density would be conducive to the preferential destruction of high-mass clusters. A purely dynamical line-of-reasoning leads therefore to a conclusion consistent with star formation a process driven by a volume density threshold. Developing this concept further, properties of molecular clumps and CFRgs naturally get dissociated. This allows to understand: (i) why the star cluster mass function is steeper than the molecular cloud (clump) mass function; (ii) the presence of a massive star formation limit in the mass-size space of molecular structures.
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