嵌入星团中分形和旋转的演化
Evolution of fractality and rotation in embedded star clusters
摘要：
越来越多的观测表明，年轻的星团可能保留着它们形成过程的印记。特别是，子结构和旋转的程度可能是这些系统形成的母体分子云崩溃的直接结果。原则上，这些性质可以被洗掉，但它们也会对这些系统的松弛产生影响。我们运行并分析了一组10个通过湍流大质量分子云坍塌形成嵌入星团的流体动力学模拟。我们系统地研究了我们的星团的分形，表明它们都是非常亚结构的（分形维数$D=1.0-1.8$）。我们还发现，随着时间的推移，分形在小尺度上缓慢减少，而在更长的时间尺度上，它在大尺度上持续存在。旋转的签名被发现在不同的模拟在每一个时间的演变，即使是轻微的监督子结构，证明母分子气体转移其角动量的一部分，以新的恒星系统。
英文摘要：
More and more observations indicate that young star clusters could retain imprints of their formation process. In particular, the degree of substructuring and rotation are possibly the direct result of the collapse of the parent molecular cloud from which these systems form. Such properties can, in principle, be washed-out, but they are also expected to have an impact on the relaxation of these systems. We ran and analyzed a set of ten hydrodynamical simulations of the formation of embedded star clusters through the collapse of turbulent massive molecular clouds. We systematically studied the fractality of our star clusters, showing that they are all extremely substructured (fractal dimension $D=1.0-1.8$). We also found that fractality is slowly reduced, with time, on small scales, while it persists on large scales on longer timescales. Signatures of rotation are found in different simulations at every time of the evolution, even for slightly supervirial substructures, proving that the parent molecular gas transfers part of its angular momentum to the new stellar systems.
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