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Laboratory Experiments, Numerical Simulations, and Astronomical Observations of Deflected Supersonic Jets: Application to HH 110

機(jī)譯：實(shí)驗室實(shí)驗，數(shù)值模擬和天文學(xué) ??偏轉(zhuǎn)超音速噴射的觀測：應(yīng)用于HH 110

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Collimated supersonic flows in laboratory experiments behave in a similarmanner to astrophysical jets provided that radiation, viscosity, and thermalconductivity are unimportant in the laboratory jets, and that the experimentaland astrophysical jets share similar dimensionless parameters such as the Machnumber and the ratio of the density between the jet and the ambient medium.Laboratory jets can be studied for a variety of initial conditions, arbitraryviewing angles, and different times, attributes especially helpful forinterpreting astronomical images where the viewing angle and initial conditionsare fixed and the time domain is limited. Experiments are also a powerful wayto test numerical fluid codes in a parameter range where the codes must performwell. In this paper we combine images from a series of laboratory experimentsof deflected supersonic jets with numerical simulations and new spectralobservations of an astrophysical example, the young stellar jet HH 110. Theexperiments provide key insights into how deflected jets evolve in 3-D,particularly within working surfaces where multiple subsonic shells andfilaments form, and along the interface where shocked jet material penetratesinto and destroys the obstacle along its path. The experiments also underscorethe importance of the viewing angle in determining what an observer will see.The simulations match the experiments so well that we can use the simulatedvelocity maps to compare the dynamics in the experiment with those implied bythe astronomical spectra. The experiments support a model where the observedshock structures in HH 110 form as a result of a pulsed driving source ratherthan from weak shocks that may arise in the supersonic shear layer between theMach disk and bow shock of the jet's working surface.
機(jī)譯：如果輻射，粘度和熱導(dǎo)率在實(shí)驗室射流中不重要，并且實(shí)驗和天體射流具有類似的無量綱參數(shù)（例如馬赫數(shù)和馬赫數(shù)之間的密度比），則實(shí)驗室實(shí)驗中準(zhǔn)直的超音速流的行為與天體射流的行為類似?？梢匝芯繉?shí)驗室射流的各種初始條件，任意視角和不同時間，這些屬性特別有助于解釋視角和初始條件固定且時域受限的天文圖像。實(shí)驗也是在數(shù)字代碼必須表現(xiàn)良好的參數(shù)范圍內(nèi)測試數(shù)字流體代碼的有效方法。在本文中，我們將來自一系列偏轉(zhuǎn)超聲速射流的實(shí)驗室實(shí)驗的圖像與數(shù)值模擬和天體物理示例（年輕的恒星射流HH 110）的新光譜觀測相結(jié)合。這些實(shí)驗提供了有關(guān)偏轉(zhuǎn)射流如何在3D模式下（尤其是在工作中）演化的關(guān)鍵見解。形成多個亞音速殼和細(xì)絲的表面，以及沿著界面的沖擊噴射材料滲透并破壞沿其路徑的障礙物。實(shí)驗還強(qiáng)調(diào)了視角對于確定觀察者所見的重要性。模擬與實(shí)驗非常匹配，因此我們可以使用模擬的速度圖將實(shí)驗中的動力學(xué)與天文光譜所暗示的動力學(xué)進(jìn)行比較。實(shí)驗支持一個模型，在該模型中，觀察到的HH 110中的沖擊結(jié)構(gòu)是脈沖驅(qū)動源形成的，而不是由馬赫圓盤之間的超音速剪切層中可能產(chǎn)生的弱沖擊和射流工作面的弓形沖擊形成的。

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