Cr–K EMISSION LINE AS A CONSTRAINT ON THE PROGENITOR PROPERTIES OF SUPERNOVA REMNANTS
Cr–K EMISSION LINE AS A CONSTRAINT ON THE PROGENITOR PROPERTIES OF SUPERNOVA REMNANTS
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DOI：
10.1088/0004-637x/766/1/44
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发表时间：
2013-02
期刊：
影响因子：
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通讯作者：
X. J. Yang;H. Tsunemi;F. Lu;Aigen Li;F. Xiang;H. Xiao;J. Zhong
中科院分区：
文献类型：
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作者：
X. J. Yang;H. Tsunemi;F. Lu;Aigen Li;F. Xiang;H. Xiao;J. Zhong
利用日本x射线天文卫星Suzaku对年轻超新星遗迹（SNRs）中的Cr、Mn和Fe-K发射谱线进行了观测。在3C 397和0519−69.0中首次检测到Cr和（或）Mn发射谱线。我们也证实了在Kepler， W49B， N103B和Cas a中检测到这些谱线。我们推导了这六个源的谱线参数（即谱线质心能量，通量和等效宽度（EW）），并对Cr， Mn和Fe的谱线中心能量进行了相关分析。相关分析还包括Tycho和G344.7−0.1，它们的Cr、Mn和Fe-K线参数通过Suzaku观测可在文献中获得。我们发现Cr的线中心能与Fe和Mn的线中心能有很好的相关性。这证实了我们之前的发现，即Cr， Mn和Fe在空间上是共存的，具有相似的电离状态，并且在超新星核合成中具有共同的起源。我们发现，Cr发射线的电子束与Fe（）的电子束之比对SNR起源和SN爆炸机制提供了有用的约束：对于γCr/Fe > %的SNR，有利于Ia型起源（如N103B， G344.7−0.1,3C 397和0519−69.0）；对于γCr/Fe < 2%的snr，它们可能是核坍缩起源或碳爆燃Ia起源。
We perform a survey of the Cr, Mn, and Fe–K emission lines in young supernova remnants (SNRs) with the Japanese X-ray astronomy satellite Suzaku. The Cr and/or Mn emission lines are detected in 3C 397 and 0519−69.0 for the first time. We also confirm the detection of these lines in Kepler, W49B, N103B, and Cas A. We derive the line parameters (i.e., the line centroid energy, flux, and equivalent width (EW)) for these six sources and perform a correlation analysis for the line center energies of Cr, Mn, and Fe. Also included in the correlation analysis are Tycho and G344.7−0.1 for which the Cr, Mn, and Fe–K line parameters were available in the literature through Suzaku observations. We find that the line center energies of Cr correlate very well with that of Fe and that of Mn. This confirms our previous findings that Cr, Mn, and Fe are spatially co-located, share a similar ionization state, and have a common origin in the supernova nucleosynthesis. We find that the ratio of the EW of the Cr emission line to that of Fe () provides useful constraints on the SNR progenitors and on the SN explosion mechanisms: for SNRs with γCr/Fe > 2%, a Type Ia origin is favored (e.g., N103B, G344.7−0.1, 3C 397, and 0519−69.0); for SNRs with γCr/Fe < 2%, they could be of either core-collapse origin or carbon-deflagration Ia origin.