Supersonic Turbulence Generated by Protostellar Outflows and Their Effects on Star Cluster Formation

最近的观测显示，星团形成于毫秒级的致密分子云团中。这项研究的目的是阐明恒星是如何在密集的星团中形成的。从三维模拟中我们发现，原恒星外流可以向周围气体注入足够的动量，从而使超音速湍流能够持续很长一段时间。所提供的湍流往往会通过压缩周围的气体来触发致密的核心形成。这样形成的岩心是在强大的外部压力的作用下形成的，因此岩心的动力演化是由外部压力控制的，而不是由自重控制的。将我们的模型与附近星系团形成区的观测结果进行比较，我们发现我们的模型能够重现观测到的核心性质。

Recent observations have revealed that star clusters form in parsec-scale dense clumps of molecular clouds. The purpose of this study is to clarify how stars form in the dense clumps. From the 3D simulations, we found that protostellar outflows can inject enough momenta into the surrounding gas and thus the supersonic turbulence can maintain for a long time. The supplied turbulence tends to trigger the dense core formation by compressing the surrounding gas. The cores so formed are exerted by the strong external pressures and thus the core dynamical evolution is controlled by the external pressure, instead of the self-gravity. Comparing between our model and observations of nearby cluster-forming regions, we found that our model can reproduce the observed core properties.