偏转超音速喷流的实验室实验、数值模拟和天文观测：对HH 110的应用
Laboratory Experiments, Numerical Simulations, and Astronomical Observations of Deflected Supersonic Jets: Application to HH 110
摘要：
实验室实验中的准直超音速流的行为与天体物理学射流的行为类似，只要辐射、粘性和热导率在实验室射流中不重要，并且实验射流和天体物理学射流具有类似的无量纲参数，如马赫数和射流与周围介质之间的密度比。实验室喷流可以在各种初始条件、任意视角和不同时间下进行研究，这些属性特别有助于解释天文图像，其中视角和初始条件是固定的，时域有限。实验也是一个强大的方法来测试数值流体代码的参数范围内的代码必须执行良好。在本文中，我们结合图像从一系列实验室实验的偏转超音速射流与数值模拟和新的光谱观测的天体物理学的例子，年轻的恒星喷流HH 110。这些实验提供了关键的见解如何偏转射流演变的3-D，特别是在工作表面内的多个亚音速壳和细丝形成，并沿界面冲击射流材料渗透到并破坏沿其路径的障碍物。实验还强调了观察角度的重要性，在确定观察者会看到什么。模拟结果与实验结果非常吻合，我们可以使用模拟的速度图来比较实验中的动力学与天文光谱所暗示的动力学。实验支持一个模型，在HH 110中观察到的激波结构的形式作为一个脉冲驱动源的结果，而不是从弱的冲击，可能会出现在超音速剪切层之间的马赫盘和弓形激波的射流的工作表面。
英文摘要：
Collimated supersonic flows in laboratory experiments behave in a similar manner to astrophysical jets provided that radiation, viscosity, and thermal conductivity are unimportant in the laboratory jets, and that the experimental and astrophysical jets share similar dimensionless parameters such as the Mach number and the ratio of the density between the jet and the ambient medium. Laboratory jets can be studied for a variety of initial conditions, arbitrary viewing angles, and different times, attributes especially helpful for interpreting astronomical images where the viewing angle and initial conditions are fixed and the time domain is limited. Experiments are also a powerful way to test numerical fluid codes in a parameter range where the codes must perform well. In this paper we combine images from a series of laboratory experiments of deflected supersonic jets with numerical simulations and new spectral observations of an astrophysical example, the young stellar jet HH 110. The experiments provide key insights into how deflected jets evolve in 3-D, particularly within working surfaces where multiple subsonic shells and filaments form, and along the interface where shocked jet material penetrates into and destroys the obstacle along its path. The experiments also underscore the importance of the viewing angle in determining what an observer will see. The simulations match the experiments so well that we can use the simulated velocity maps to compare the dynamics in the experiment with those implied by the astronomical spectra. The experiments support a model where the observed shock structures in HH 110 form as a result of a pulsed driving source rather than from weak shocks that may arise in the supersonic shear layer between the Mach disk and bow shock of the jet's working surface.
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