分子云中分布和离散星的形成
The Formation of Distributed and Clustered Stars in Molecular Clouds
摘要：
在过去的二十年里，恒星形成研究的重点已经从理解单个致密核心坍缩成恒星转移到研究分子云中数百至数千颗恒星的形成。在这一章中，我们综述了最近的观测和理论进展，了解恒星形成的分子云和复合物的规模，即恒星形成的宏观物理。我们首先概述了最近调查的年轻恒星天体（YSO）的分子云和嵌入式集群，我们概述了一个新兴的图片团簇形成。然后，我们讨论了湍流的作用，既支持云，创造密集的，引力不稳定的结构，强调磁场（在分布式恒星的情况下）和反馈（在集群的情况下）的作用，以减缓湍流衰减和调解的速度和密度的恒星形成。讨论之后是一个概述如何重力和湍流可能会产生观察到的分子云，恒星和星团的性质的标度律，以及如何观察到，低恒星形成率可能会导致自我调节恒星形成。最后，我们提出一些结论性意见，包括一些有待于今后观察和模拟解决的问题。
英文摘要：
During the last two decades, the focus of star formation research has shifted from understanding the collapse of a single dense core into a star to studying the formation hundreds to thousands of stars in molecular clouds. In this chapter, we overview recent observational and theoretical progress toward understanding star formation on the scale of molecular clouds and complexes, i.e the macrophysics of star formation. We begin with an overview of recent surveys of young stellar objects (YSOs) in molecular clouds and embedded clusters, and we outline an emerging picture of cluster formation. We then discuss the role of turbulence to both support clouds and create dense, gravitationally unstable structures, with an emphasis on the role of magnetic fields (in the case of distributed stars) and feedback (in the case of clusters) to slow turbulent decay and mediate the rate and density of star formation. The discussion is followed by an overview of how gravity and turbulence may produce observed scaling laws for the properties of molecular clouds, stars and star clusters, and how the observed, low star formation rate may result from self regulated star formation. We end with some concluding remarks, including a number of questions to be addressed by future observations and simulations.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
