Suzaku discovery of Fe K-shell line from the O-rich SNR G292.0+1.8
Suzaku discovery of Fe K-shell line from the O-rich SNR G292.0+1.8
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DOI：
10.1093/pasj/psu035
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发表时间：
2014-02
影响因子：
2.3
通讯作者：
F. Kamitsukasa;K. Koyama;H. Tsunemi;K. Hayashida;H. Nakajima;H. Takahashi;S. Ueda;K. Mori;S. Katsuda;H. Uchida
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文献类型：
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作者：
F. Kamitsukasa;K. Koyama;H. Tsunemi;K. Hayashida;H. Nakajima;H. Takahashi;S. Ueda;K. Mori;S. Katsuda;H. Uchida
我们报告了银河系富氧超新星遗迹（SNR）G292.0+1.8（核心塌陷超新星遗迹）的朱雀/XIS 结果。 G292.0+1.8的X射线谱由两种类型的等离子体组成，一种处于碰撞电离平衡（CIE），另一种处于非平衡电离（NEI）。 CIE 等离子体的丰度接近太阳，因此可能起源于星周和星际介质。 NEI等离子体具有超太阳丰度，丰度模式表明该等离子体起源于主序带为30-35 Msolar的超新星喷射物。首次在 NEI 等离子体中检测到能量为 6.6 keV 的铁 K 壳线。
We report the Suzaku/XIS results of the Galactic oxygen-rich supernova remnant (SNR), G292.0+1.8, a remnant of a core-collapse supernova. The X-ray spectrum of G292.0+1.8 consists of two type plasmas, one is in collisional ionization equilibrium (CIE) and the other is in non-equilibrium ionization (NEI). The CIE plasma has nearly solar abundances, and hence would be originated from the circumstellar and interstellar mediums. The NEI plasma has super-solar abundances, and the abundance pattern indicates that the plasma originates from the supernova ejecta with a main sequence of 30-35 Msolar. Iron K-shell line at energy of 6.6 keV is detected for the first time in the NEI plasma.