The physics and modes of star cluster formation: simulations
The physics and modes of star cluster formation: simulations
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星团形成的物理和模式：模拟
DOI：
10.1098/rsta.2009.0262
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发表时间：
2009
期刊：
影响因子：
--
通讯作者：
C. Clarke
中科院分区：
文献类型：
--
作者：
C. Clarke
综述了星星团形成的数值模拟研究进展。这些模拟涉及自下而上的集群组装通过分级合并，这产生了一个分形恒星分布在年轻（约。0.5 Myr）年龄。由此产生的集群被预测为轻度非球面和高度质量分离，除了在合并后立即。在个别集群内的上初始质量函数通常比总人口略平坦。最近的工作已经开始阐明控制恒星形成云中恒星平均质量的因素，以及星星形成的效率。前者对气体的热性质敏感，而后者则依赖于磁场和纳塔尔云的初始引力束缚度。最初束缚在一起的非磁化云会迅速坍缩，这很难通过电离反馈或恒星风来逆转。
We review progress in numerical simulations of star cluster formation. These simulations involve the bottom-up assembly of clusters through hierarchical mergers, which produces a fractal stellar distribution at young (approx. 0.5 Myr) ages. The resulting clusters are predicted to be mildly aspherical and highly mass-segregated, except in the immediate aftermath of mergers. The upper initial mass function within individual clusters is generally somewhat flatter than for the aggregate population. Recent work has begun to clarify the factors that control the mean stellar mass in a star-forming cloud and also the efficiency of star formation. The former is sensitive to the thermal properties of the gas while the latter depends both on the magnetic field and the initial degree of gravitational boundedness of the natal cloud. Unmagnetized clouds that are initially bound undergo rapid collapse, which is difficult to reverse by ionization feedback or stellar winds.
恒星形成对初始条件和分子云结构的依赖性
DOI：
10.1111/j.1365-2966.2009.14970.x
发表时间：
2009
影响因子：
4.8
作者：
Bate M
通讯作者：
Bate M