共生星MWC 560中喷流的流体动力学模拟。II。超越密度平衡的模拟
Hydrodynamical simulations of the jet in the symbiotic star MWC 560. II. Simulations beyond density balance
摘要：
（摘要）在本系列的第一篇论文中，我们提出了具有共生系统MWC 560的参数代表的射流模型的辐射冷却的流体动力学模拟。这些是在高密度环境介质中的脉冲式、初始欠密度射流的射流模拟。当喷气式飞机达到50 AU的长度时，他们停了下来。然而，在那里，最初的低密度射流向高密度射流的过渡应该发生，这应该导致运动学的改变。因此，我们描述了两个流体动力学模拟与冷却超过这个密度平衡，一个具有相同的参数作为模型i在论文I（现在称为模型i '），这是有和没有冷却，第二个与更高的气体密度在射流脉冲（模型iv'）。流体动力学模拟，与进一步近似的冷却处理相比，纸我，被用来能够扩大计算域。这种转变导致茧的膨胀发生变化，从而导致射流形态发生变化，例如射流结的径向宽度变大。我们调查的射流，韧致辐射和光学发射率，综合发射图，和合成吸收线轮廓的辐射特性。天鹅座CH、宝瓶座R和MWC 560中观测到的高速度有利于冷却模型的结论没有被转变改变。在宝瓶座R观测到的平行特征可以由内部结或由冲击环境介质的可变密集辐射壳产生。吸收线的分布表明，MWC 560中的实际参数更接近模型iv'而不是模型i'。
英文摘要：
(Abridged) In the first paper of this series, we presented hydrodynamical simulations with radiative cooling of jet models with parameters representative of the symbiotic system MWC 560. These were jet simulations of a pulsed, initially underdense jet in a high-density ambient medium. They were stopped when the jet reached a length of 50 AU. There, however, a transition of the initially underdense jet towards an overdense jet should occur, which should result in changed kinematics. Therefore, we describe two hydrodynamical simulations with cooling beyond this density balance, one with the same parameters as model i in Paper I (now called model i'), which was presented there with and without cooling, and the second with higher gas densities in the jet pulses (model iv'). Hydrodynamical simulations, with a further approximated cooling treatment compared to Paper I, were used to be able to enlarge the computational domain. The transition causes changes in the expansion of the cocoon and therefore the morphology of the jet, e.g. a larger radial width of the jet knots. We investigate the radiation properties of the jets, the bremsstrahlung and optical emissivities, integrated emission maps, and synthetic absorption line profiles. The conclusion that the high observed velocities in CH Cygni, R Aquarii, and MWC 560 favor the models with cooling is unchanged by the transition. The observed parallel features in R Aquarii can be produced by the internal knots or by a variable dense radiative shell of shocked ambient medium. The absorption line profiles show that the real parameters in MWC 560 are closer to model iv' than to model i'.
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