论文标题
磁场与丝状云之间的联系III：场调节的质量累积功能
The links between magnetic fields and filamentary clouds III: field regulated mass cumulative functions
论文作者
论文摘要
在过去的十年中，随着观察证据的积累，磁场在分子云中的动态重要性越来越多。但是，磁场如何影响恒星形成仍不清楚。典型的恒星形成模型仍然将磁场视为各向同性压力，忽略了动态重要的磁场的基本特性：它们的方向。这项研究以我们先前的工作为基础，该工作证明了相对于全球云伸长的平均磁场方向如何影响云碎片。在前面报告的线性质量分布之后，我们在这里表明云的质量累积函数（MCF）也受现场取向调节。靠近田间方向的云延伸倾向于具有较浅的MCF，换句话说，高密度的气体的较高部分。证据与我们对前面发现的双峰恒星形成效率的理解一致，这也与田间方向相关。
During the past decade the dynamical importance of magnetic fields in molecular clouds has been increasingly recognized, as observational evidence has accumulated. However, how a magnetic field affect star formation is still unclear. Typical star formation models still treat a magnetic fields as an isotropic pressure, ignoring the fundamental property of dynamically important magnetic fields: their direction. This study builds on our previous work which demonstrated how the mean magnetic field orientation relative to the global cloud elongation can affect cloud fragmentation. After the linear mass distribution reported earlier, we show here that the mass cumulative function (MCF) of a cloud is also regulated by the field orientation. A cloud elongated closer to the field direction tends to have a shallower MCF, in other words, a higher portion of the gas in high density. The evidence is consistent with our understanding of bimodal star formation efficiency discovered earlier, which is also correlated with the field orientations.
