Far-Ultraviolet and X-Ray Observations of the Reverse Shock in the Small Magellanic Cloud Supernova Remnant 1E 0102.2–7219
Far-Ultraviolet and X-Ray Observations of the Reverse Shock in the Small Magellanic Cloud Supernova Remnant 1E 0102.2–7219
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小麦哲伦星云超新星遗迹 1E 0102.2–7219 中反向激波的远紫外和 X 射线观测
DOI：
10.1086/500789
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发表时间：
2006
期刊：
影响因子：
--
通讯作者：
Randall K. Smith
中科院分区：
文献类型：
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作者：
M. Sasaki;T. Gaetz;W. Blair;R. Edgar;J. Morse;P. Plucinsky;Randall K. Smith
本文介绍了小麦哲伦星云中富氧超新星遗迹1 E 0102.2-7219的反激波的远紫外光谱探测器（FUSE）和X射线多镜使命任务（XMM-牛顿）数据。FUSE观测覆盖了三个具有显著不同光学[O III]强度的区域，所有这些区域都与X射线环相对明亮的部分有关。在FUSE光谱中清晰地检测到OVI λλ1032、1038发射线。XMM-牛顿EPIC MOS 1/2光谱由O、Ne和Mg的强发射线主导。将O-VI双重态发射与O-VII三重态和O-VIII Lyα通量结合起来，并假设谱图为单电离时标的非平衡电离（NEI）模型，我们发现电离时标τ从北（τ = 0.6 × 1011 s cm-3）向东南（τ = 2 × 1011 s cm-3）增加。这表明X射线亮环中的密度增加，与东南部最强的光学[O III]发射非常一致。然而，如果我们假设一个平面平行冲击模型的电离时标的分布，O VI的排放似乎是不一致的O VII和O VIII的X射线。总的X射线光谱的分析表明，没有一组一致的值的温度和电离时间尺度，可以解释所观察到的线比为O，Ne，和Mg。这与喷出物的结构性分布是一致的，因为O、Ne和Mg会在不同的时间与反向冲击相互作用。
We present Far Ultraviolet Spectroscopic Explorer (FUSE) and X-Ray Multi-Mirror Mission (XMM-Newton) data for the reverse shock of the O-rich supernova remnant (SNR) 1E 0102.2-7219 in the Small Magellanic Cloud (SMC). The FUSE observations cover three regions with significantly different optical [O III] intensities, all associated with the relatively bright part of the X-ray ring. Emission lines of O VI λλ1032, 1038 are clearly detected in the FUSE spectra. The XMM-Newton EPIC MOS 1/2 spectra are dominated by strong emission lines of O, Ne, and Mg. By combining the O VI doublet emission with the O VII triplet and O VIII Lyα fluxes from the X-ray spectra and assuming a nonequilibrium ionization (NEI) model with a single ionization timescale for the spectra, we find an increase of the ionization timescale τ from north (τ ≈ 0.6 × 1011 s cm-3) to southeast (τ ≈ 2 × 1011 s cm-3). This is indicative of increasing density in the X-ray-bright ring, in good agreement with the optical [O III] emission, which is strongest in the southeast. However, if we assume a plane-parallel shock model with a distribution of ionization timescales, the O VI emission appears to be inconsistent with O VII and O VIII in X-rays. The analysis of the total X-ray spectra shows that there is no consistent set of values for the temperature and ionization timescale that can explain the observed line ratios for O, Ne, and Mg. This would be consistent with a structured distribution of the ejecta, as the O, Ne, and Mg would have interacted with the reverse shock at different times.