水螅A中的喷流-团内介质相互作用。I从内结估算射流速度
Jet-Intracluster Medium interaction in Hydra A. I Estimates of jet velocity from inner knots
摘要：
我们提出的第一阶段的调查的相互作用的喷流在射电星系长蛇座A与集群内的介质。我们考虑喷流动能，星系和星团大气，以及射电源的内部结构。通过分析Taylor等人（1990）对Hydra A内叶的射电观测，我们证实了Wise等人（2007）从X射线腔的动力学分析中得出的喷流功率估计约为1 e45 ergs/s。有了这个结果和星系晕的模型，我们探索的射流内集群介质的相互作用发生在一个规模为10千秒差距，使用二维，轴对称，相对论纯流体动力学模拟。一个关键的特点是，我们确定了三个明亮的结在北方的射流作为双锥约束冲击，这导致当一个过压射流开始进入平衡与银河系大气。通过对参数空间的研究，我们推断出在距离黑洞0.5千秒差距处喷流的速度约为0.8摄氏度。喷流功率、沿喷流观察到的喷流半径剖面以及估计的喷流压力和喷流速度的组合约束意味着北喷流的喷流密度参数值约为13。我们发现，对于喷流速度= 0.8c和喷流和视线之间的角度= 42度，在北部和南部喷流的发射率的内在不对称性是需要一个一致的亮度比约7估计从6厘米VLA图像的水螅A。
英文摘要：
We present the first stage of an investigation of the interactions of the jets in the radio galaxy Hydra A with the intracluster medium. We consider the jet kinetic power, the galaxy and cluster atmosphere, and the inner structure of the radio source. Analysing radio observations of the inner lobes of Hydra A by Taylor et al. (1990) we confirm the jet power estimates of about 1e45 ergs/s derived by Wise et al. (2007) from dynamical analysis of the X-ray cavities. With this result and a model for the galaxy halo, we explore the jet-intracluster medium interactions occurring on a scale of 10 kpc using two-dimensional, axisymmetric, relativistic pure hydrodynamic simulations. A key feature is that we identify the three bright knots in the northern jet as biconical reconfinement shocks, which result when an over pressured jet starts to come into equilibrium with the galactic atmosphere. Through an extensive parameter space study we deduce that the jet velocity is approximately 0.8 c at a distance 0.5 kpc from the black hole. The combined constraints of jet power, the observed jet radius profile along the jet, and the estimated jet pressure and jet velocity imply a value of the jet density parameter approximately 13 for the northern jet. We show that for a jet velocity = 0.8c and angle between the jet and the line of sight = 42 deg, an intrinsic asymmetry in the emissivity of the northern and southern jet is required for a consistent brightness ratio approximately 7 estimated from the 6cm VLA image of Hydra A.
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