X-Ray Signatures of Evolving Radio Galaxies
X-Ray Signatures of Evolving Radio Galaxies
复制标题
演化射电星系的 X 射线特征
DOI：
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发表时间：
1998
期刊：
影响因子：
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通讯作者：
M. Begelman
中科院分区：
文献类型：
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作者：
S. Heinz;C. Reynolds;M. Begelman
我们提出了一个简单的模型，一个不断发展的无线电星系，因为它扩展到热，X射线发射星际介质（ISM）的宿主星系或类似的热团内介质（ICM）的宿主集群。我们数值求解控制方程的网格模型参数，以提出简单的分析工具，被推出的茧和相关的腔在集群发射的冲击壳的X射线观测。我们将这些工具应用于英仙座A的著名例子，表明其时间平均动力学光度可能超过1046尔格s-1，远大于估计的电流功率。我们展示了如何未来的观测可以用来提取有用的源参数，如平均动力学功率和源年龄，并讨论在其生命的各个阶段的源的可探测性。
We present a simple model for an evolving radio galaxy as it expands into the hot, X-ray-emitting interstellar medium (ISM) of its host galaxy or similarly into the hot intracluster medium (ICM) of its host cluster. We solve the governing equations numerically on a grid of model parameters in order to present simple analytical tools for X-ray observations of the shocked shell that is pushed out by the cocoon and the associated cavity in the cluster emission. We apply these tools to the well-known example of Perseus A to show that its time-averaged kinetic luminosity probably exceeds 1046 ergs s-1, much larger than the estimated current power. We show how future observations can be used to extract useful source parameters such as the average kinetic power and the source age, and discuss detectability of sources at various stages of their lives.