LINE-OF-SIGHT SHELL STRUCTURE OF THE CYGNUS LOOP
LINE-OF-SIGHT SHELL STRUCTURE OF THE CYGNUS LOOP
复制标题
天鹅座环的视线壳结构
DOI：
10.1088/0004-637x/705/2/1152
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发表时间：
2009
期刊：
影响因子：
--
通讯作者：
H. Takahashi
中科院分区：
文献类型：
--
作者：
H. Uchida;H. Tsunemi;S. Katsuda;M. Kimura;H. Kosugi;H. Takahashi
我们利用朱雀和XMM-牛顿卫星获得的41个观测数据对天鹅座环的壳结构进行了全面研究。为了研究天鹅座环的详细等离子体结构，我们将视野划分为 1042 个盒子区域。从光谱分析来看，从环路肢体获得的光谱与单组分非平衡电离等离子体模型很好地拟合。另一方面，从内部区域获得的光谱与二元模型很好地拟合。结果，我们确认低温和高温成分分别源自周围的星际物质（ISM）和环路的喷射物。根据最佳拟合结果，我们显示了 ISM 组件的通量分布。分布清楚地显示了肢体增亮结构，我们发现了一些低通量区域。其中，南部井喷地区流量最低。我们还在中心偏西和东北发现了其他大片低通量区域。我们估计前薄壳区域的直径约为 1.°3，并得出结论，除了南面井喷之外，沿视线还存在井喷。我们还计算了ISM组件的排放测度分布，结果表明Cygnus Loop与简单Sedov演化模型得到的结果相去甚远。从结果来看，我们支持天鹅座环起源于空腔爆炸。排放测量分布还表明，东北部的空腔壁密度高于西南部。这些结果表明天鹅座环周围的空腔壁的厚度不均匀。
We conducted a comprehensive study on the shell structure of the Cygnus Loop using 41 observation data obtained by the Suzaku and the XMM-Newton satellites. To investigate the detailed plasma structure of the Cygnus Loop, we divided our fields of view into 1042 box regions. From the spectral analysis, the spectra obtained from the limb of the Loop are well fitted by the single-component non-equilibrium ionization plasma model. On the other hand, the spectra obtained from the inner regions are well fitted by the two-component model. As a result, we confirmed that the low-temperature and high-temperature components originated from the surrounding interstellar matter (ISM) and the ejecta of the Loop, respectively. From the best-fit results, we showed a flux distribution of the ISM component. The distribution clearly shows the limb-brightening structure, and we found out some low-flux regions. Among them, the south blowout region has the lowest flux. We also found other large low-flux regions at slightly west and northeast from the center. We estimated the former thin shell region to be ∼1.°3 in diameter and concluded that there exists a blowout along the line of sight in addition to the south blowout. We also calculated the emission measure distribution of the ISM component and showed that the Cygnus Loop is far from the result obtained by a simple Sedov evolution model. From the results, we support that the Cygnus Loop originated from a cavity explosion. The emission measure distribution also suggests that the cavity-wall density is higher in the northeast than that in the southwest. These results suggest that the thickness of the cavity wall surrounding the Cygnus Loop is not uniform.
DOI：
10.1086/523263
发表时间：
2007-10
期刊：
The Astrophysical Journal
影响因子：
--
作者：
H. Tsunemi;S. Katsuda;N. Nemes;E. Miller
通讯作者：
H. Tsunemi;S. Katsuda;N. Nemes;E. Miller
地球磁鞘太阳风电荷交换 X 射线发射的证据
DOI：
--
发表时间：
2007
期刊：
Publ.Astron.So.c.Japan 59SP1
影响因子：
--
作者：
R. Fujimoto;K. Mitsuda;D. McCammon;Y. Takei;M. Bauer;Y. Ishisaki;ほか
通讯作者：
ほか