X-Ray Observations of the W 51 Complex with Suzaku
X-Ray Observations of the W 51 Complex with Suzaku
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DOI：
10.1093/pasj/65.2.42
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发表时间：
2012-12
影响因子：
2.3
通讯作者：
Y. Hanabata;M. Sawada;H. Katagiri;A. Bamba;Y. Fukazawa
中科院分区：
文献类型：
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作者：
Y. Hanabata;M. Sawada;H. Katagiri;A. Bamba;Y. Fukazawa
我们用Suzaku对中年超新星遗迹w51 C和恒星形成区w51 B的x射线辐射进行了详细的分析。w51 C的软x射线发射可以很好地表征为温度为0.7 keV的非平衡电离态的光学薄热等离子体。镁元素丰度显著高于太阳值。我们发现w51 c中没有明显的过电离等离子体特征，硬x射线发射在空间上与w51 B相关的分子云一致，与w51 c重叠，光谱由温度为- 5 keV的光学薄热等离子体或光子指数为- 2.2的幂律模型表示。发射可能具有漫射性质，因为它在0.5-10 keV波段的亮度为1 - 10 - 34 erg - 1，无法用该区域的任何点源发射来解释。我们讨论了硬x射线发射来自w51b中OB恒星的恒星风或加速的可能性
We present a detailed analysis of X-ray emission from the middle-aged supernova remnant W 51 C and starforming region W 51 B with Suzaku. The soft X-ray emission from W 51 C is well-represented by an optically thin thermal plasma in a non-equilibrium ionization state with a temperature of � 0.7 keV. The elemental abundance of Mg is significantly higher than the solar value. We find no significant feature of an over-ionized plasma in W 51 C. The hard X-ray emission is spatially coincident with the molecular clouds associated with W 51 B, overlapping with W 51 C. The spectrum is represented by an optically thin thermal plasma with a temperature of � 5 keV, or a powerlaw model with a photon index of � 2.2. The emission probably has a diffuse nature, since its luminosity of 1 � 10 34 erg s � 1 in the 0.5–10 keV band cannot be explained by any emission from point sources in this region. We discuss the possibility that the hard X-ray emission comes from stellar winds of OB stars in W 51 B, or accelerated