恒星形成的不确定原理。I.为什么银河系恒星形成关系在一定的空间尺度下破裂
An uncertainty principle for star formation. I. Why galactic star formation relations break down below a certain spatial scale
摘要：
星系尺度之间的关系（表面密度）的气体质量和恒星形成（SF）率被称为发展实质性的散射，甚至改变形式时，考虑低于一定的空间尺度。我们量化这种行为应该如何预期由于独立的恒星形成区域的不完全统计抽样。其他包括限制因素是不完整的采样SF示踪剂从恒星初始质量函数和气体和恒星之间的空间漂移。我们提出了一个简单的SF的不确定原理，它可以用来预测和解释银河系SF关系在小空间尺度上的失败。这种不确定原理解释了SF关系的分散如何取决于空间尺度，并预测了当将孔径集中在气体或SF示踪剂峰上时，气体耗尽时间尺度的尺度依赖性偏差。我们展示了散射和偏差如何对SF过程中所涉及的物理大小和时间尺度（如其持续时间或分子云寿命）敏感，并说明了我们的形式主义如何提供了一个强大的工具来约束这些基本上未知的量。由于它的一般形式，不确定原理也可以应用于其他天体物理系统，例如解决恒星形成核心，原行星盘或星系及其核的时间演化。
英文摘要：
Galactic scaling relations between the (surface densities of) the gas mass and the star formation (SF) rate are known to develop substantial scatter or even change form when considered below a certain spatial scale. We quantify how this behaviour should be expected due to the incomplete statistical sampling of independent star-forming regions. Other included limiting factors are the incomplete sampling of SF tracers from the stellar initial mass function and the spatial drift between gas and stars. We present a simple uncertainty principle for SF, which can be used to predict and interpret the failure of galactic SF relations on small spatial scales. This uncertainty principle explains how the scatter of SF relations depends on the spatial scale and predicts a scale-dependent bias of the gas depletion time-scale when centering an aperture on gas or SF tracer peaks. We show how the scatter and bias are sensitive to the physical size and time-scales involved in the SF process (such as its duration or the molecular cloud lifetime), and illustrate how our formalism provides a powerful tool to constrain these largely unknown quantities. Thanks to its general form, the uncertainty principle can also be applied to other astrophysical systems, e.g. addressing the time-evolution of star-forming cores, protoplanetary discs, or galaxies and their nuclei.
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