论文标题
物理特性和分子云的缩放关系：恒星形成的影响
Physical Properties and Scaling Relations of Molecular Clouds: the Impact of Star Formation
论文作者
论文摘要
使用银河系状星系的流体动力学模拟，达到4.6 PC分辨率，我们研究了恒星形成标准的选择如何影响银河系和巨型分子云（GMC）尺度。我们发现，与使用分子星形形成方法相比，使用湍流，自我塑造的恒星形成标准会导致密度在10到10 $^4 $ cm $^{ - 3} $之间的气体比例增加，尽管既有几乎相同的气态和恒星形态。此外，我们发现恒星形成的位置是由前者倾向于仅在非常高密度（$ \ gt 10 $ cm $ $^{ - 3} $）气体的区域中产生的星星的恒星，而后者则在其螺旋臂的整个长度上形成恒星。 GMC的特性受到恒星形成标准的选择，而前者产生了较大的云。尽管存在差异，我们发现云属性之间的关系（例如拉尔森关系）仍然不受影响。最后，GMC的每个自由下降时间的测得的星形形成效率中的散射仍然存在两种方法，因此由其他因素设定。
Using hydrodynamical simulations of a Milky Way-like galaxy, reaching 4.6 pc resolution, we study how the choice of star formation criteria impacts both galactic and Giant Molecular Clouds (GMC) scales. We find that using a turbulent, self-gravitating star formation criteria leads to an increase in the fraction of gas with densities between 10 and 10$^4$ cm$^{-3}$ when compared with a simulation using a molecular star formation method, despite both having nearly identical gaseous and stellar morphologies. Furthermore, we find that the site of star formation is effected with the the former tending to only produce stars in regions of very high density ($\gt 10$ cm$^{-3}$) gas while the latter forms stars along the entire length of its spiral arms. The properties of GMCs are impacted by the choice of star formation criteria with the former method producing larger clouds. Despite the differences we find that the relationships between clouds properties, such as the Larson relations, remain unaffected. Finally, the scatter in the measured star formation efficiency per free-fall time of GMCs remains present with both methods and is thus set by other factors.
