中龄超新星遗迹G156 .2+5.7的热和非热X射线辐射的朱雀观测
Suzaku Observations of Thermal and Non-Thermal X-Ray Emission from the Middle-Aged Supernova Remnant G156.2+5.7
摘要：
本文介绍了银河系中龄超新星遗迹（SNR）G156.2+5.7的X射线分析结果。该超新星遗迹明亮，在X射线波长上有很大的扩展，呈明显的圆形（半径约50 '）。使用朱雀卫星，我们在三个点观察到这个SNR;部分覆盖西北边缘，东部边缘和这个SNR的中心部分。在西北缘和中部，我们确认X射线谱包括软尾和硬尾发射，而在东缘，我们没有发现显着的硬尾发射。非平衡电离（NEI）模型很好地拟合了软发射。在中心部分，一个两个组件（星际介质和富含金属的喷出物）NEI模型更适合软发射比一个单组件NEI模型从统计的角度来看。G156.2+5.7的相对丰度表明它是一个起源质量小于15M_solar的超新星爆发的残余物。硬尾辐射的起源很可能是相对论电子的非热同步辐射。在西北边缘，相对论电子似乎被一个速度约为500公里/秒的前向激波加速。
英文摘要：
We present results from X-ray analysis of a Galactic middle-aged supernova remnant (SNR) G156.2+5.7 which is bright and largely extended in X-ray wavelengths, showing a clear circular shape (radius about 50'). Using the Suzaku satellite, we observed this SNR in three pointings; partially covering the northwestern rim, the eastern rim, and the central portion of this SNR. In the northwestern rim and the central portion, we confirm that the X-ray spectra consist of soft and hard-tail emission, while in the eastern rim we find no significant hard-tail emission. The soft emission is well fitted by non-equilibrium ionization (NEI) model. In the central portion, a two-component (the interstellar medium and the metal-rich ejecta) NEI model fits the soft emission better than a one-component NEI model from a statistical point of view. The relative abundances in the ejecta component suggest that G156.2+5.7 is a remnant from a core-collapse SN explosion whose progenitor mass is less than 15 M_solar. The origin of the hard-tail emission is highly likely non-thermal synchrotron emission from relativistic electrons. In the northwestern rim, the relativistic electrons seem to be accelerated by a forward shock with a slow velocity of about 500 km/sec.
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