Star Cluster Formation and Feedback
Star Cluster Formation and Feedback
复制标题
星团的形成和反馈
DOI：
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发表时间：
2014
期刊：
影响因子：
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通讯作者：
Qizhou Zhang
中科院分区：
文献类型：
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作者：
M. Krumholz;M. Bate;H. Arce;J. Dale;R. Gutermuth;R. Klein;Zhi;F. Nakamura;Qizhou Zhang
恒星通常不是孤立形成的。相反，它们形成于星团中，在这些星团环境中，新生恒星可以对彼此及其母气体云产生深远的影响。来自星团恒星的反馈几乎肯定是造成星星形成的一些令人困惑的事实的原因：这是一个低效的过程，在银河系尺度上平均起来进展缓慢;大多数恒星从它们的诞生地分散并在时间尺度上溶解到银河系中;新生恒星遵循初始质量函数（IMF），其峰值在0.1 - 1$ $M_\odot$范围内，而不是由褐矮星主导的IMF。在这篇综述中，我们总结了目前的观测限制和理论模型之间的复杂的相互作用集群星星的形成和反馈。
Stars do not generally form in isolation. Instead, they form in clusters, and in these clustered environments newborn stars can have profound effects on one another and on their parent gas clouds. Feedback from clustered stars is almost certainly responsible for a number of otherwise puzzling facts about star formation: that it is an inefficient process that proceeds slowly when averaged over galactic scales; that most stars disperse from their birth sites and dissolve into the galactic field over timescales $\ll 1$ Gyr; and that newborn stars follow an initial mass function (IMF) with a distinct peak in the range $0.1 - 1$ $M_\odot$, rather than an IMF dominated by brown dwarfs. In this review we summarize current observational constraints and theoretical models for the complex interplay between clustered star formation and feedback.