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首页> 外文期刊>The Astrophysical journal >HYDRODYNAMICAL SIMULATIONS OF THE JET IN THE SYMBIOTIC STAR MWC 560. Ⅲ. APPLICATION TO X-RAY JETS IN SYMBIOTIC STARS
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HYDRODYNAMICAL SIMULATIONS OF THE JET IN THE SYMBIOTIC STAR MWC 560. Ⅲ. APPLICATION TO X-RAY JETS IN SYMBIOTIC STARS

机译：象征星MWC 560中射流的水力动力学模拟。在符号星的X射线射束中的应用

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摘要

In PapersⅠand Ⅱ in this series, we presented hydrodynamical simulations of jet models with parameters representative of the symbiotic system MWC 560. These were simulations of a pulsed, initially underdense jet in a high-density ambient medium. Since the pulsed emission of the jet creates internal shocks and since the jet velocity is very high, the jet bow shock and the internal shocks are heated to high temperatures and should therefore emit X-ray radiation. In this paper, we investigate in detail the X-ray properties of the jets in our models. We have focused our study on the total X-ray luminosity and its temporal variability, the resulting spectra, and the spatial distribution of the emission. Temperature aad density maps from our hydrodynamical simulations with radiative cooling presented in the second paper are used, together with emissivities calculated with the atomic database ATOMDB. The jets in our models show extended and variable X-ray emission, which can be characterized as a sum of hot and warm components with temperatures that are consistent with observations of CH Cyg and R Aqr. The X-ray spectra of our model jets show emission-line features that correspond to observed features in the spectra of CH Cyg. The innermost parts of our pulsed jets show iron line emission in the 6.4-6.7 keV range, which may explain such emission from the central source in R Aqr. We conclude that MWC 560 should be detectable with Chandra or XMM-Newton, and such X-ray observations will prove crucial for understanding jets in symbiotic stars.
机译：在该系列的论文Ⅰ和Ⅱ中，我们介绍了具有代表共生系统MWC 560的参数的射流模型的流体动力学模拟。这些模拟是在高密度环境介质中最初为脉冲的低密度射流的模拟。由于射流的脉冲发射会产生内部冲击，并且由于射流速度非常高，因此射流弓激波和内部冲击会被加热到高温，因此应该发出X射线辐射。在本文中，我们将详细研究模型中射流的X射线特性。我们将研究重点放在了总X射线发光度及其时间变异性，所产生的光谱以及发射的空间分布上。使用了第二篇论文中通过辐射冷却进行水动力模拟得到的温度和密度图，以及通过原子数据库ATOMDB计算出的发射率。我们模型中的射流显示出扩展且可变的X射线发射，其特征可以是温度与CH Cyg和R Aqr观测值一致的热和热成分之和。我们的模型喷气机的X射线光谱显示出发射谱线特征，与CH Cyg光谱中观察到的特征相对应。我们脉冲射流的最内部显示出的铁线发射范围为6.4-6.7 keV，这可以解释来自R Aqr中心源的这种发射。我们得出的结论是，钱德拉或XMM-牛顿应该可以检测到MWC 560，并且这种X射线观察将证明对理解共生恒星中的喷射至关重要。

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