星团冷核中的暖射线
Warming rays in cluster cool cores
摘要：
我们提出了一个宇宙射线加热星系团核心的模型，该模型通过使用能量平衡条件再现了星系团中观测到的温度分布，在该条件下，发射的X射线能量由强子宇宙射线提供，这些宇宙射线充当暖射线（WR）。IC气体的温度分布与WR压力分布相关，因此与WR与IC气体和磁场的相互作用引起的非热发射（无线电、硬X射线和伽马射线）相关。根据测量的离子气体密度分布，成功地预测了冷芯团簇和非冷芯团簇中离子气体的温度分布。在此约束下，WR模型也能再现团簇中的热压力和非热压力分布，以及团簇的径向熵分布。WR模型提供了其他可观察的特征：压力比的相关性（WR到热IC气体）与内部星系团温度T_{inner}、伽马射线光度与T_{inner}的相关性、通过GLAST-LAT实验可观察到的大量冷核星系团、冷核星系团中射电晕的表面亮度恢复了观察到的亮度，来自冷核星系团的硬X射线发射，系统性地低于观察到的极限，但可以通过下一代HXR实验（如Simbol-X）观察到。分析了电磁场的理论特性和多频分布。WR模型中预测的信号使它与其他提出的用于加热团簇冷核的模型有很大的不同。这种差异使得证明或反驳我们的模型作为一个解释的冷却流问题的基础上的多频观测的星系团。
英文摘要：
We present a model of cosmic ray heating of clusters' cores that reproduces the observed temperature distribution in clusters by using an energy balance condition in which the emitted X-ray energy is supplied by the hadronic cosmic rays, which act as warming rays (WRs). The temperature profile of the IC gas is correlated with the WR pressure distribution and, consequently, with the non-thermal emission (radio, hard X-ray and gamma-ray) induced by the interaction of the WRs with the IC gas and magnetic field. The temperature distribution of the IC gas in both cool-core and non cool-core clusters is successfully predicted from the measured IC gas density distribution. Under this contraint, the WR model is also able to reproduce the thermal and non-thermal pressure distribution in clusters, as well as their radial entropy distribution. The WR model provides other observable features: a correlation of the pressure ratio (WRs to thermal IC gas) with the inner cluster temperature T_{inner}, a correlation of the gamma-ray luminosity with T_{inner}, a substantial number of cool-core clusters observable with the GLAST-LAT experiment, a surface brightness of radio halos in cool-core clusters that recovers the observed one, a hard X-ray emission from cool-core clusters that is systematically lower than the observed limits and yet observable with the next generation HXR experiments like Simbol-X. The specific theoretical properties and the multi-frequency distribution of the e.m. signals predicted in the WR model render it quite different from the other models proposed for the heating of clusters' cool-cores. Such differences make it possible to prove or disprove our model as an explanation of the cooling-flow problems on the basis of multi-frequency observations of galaxy clusters.
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