EVIDENCE FOR THERMAL X-RAY LINE EMISSION FROM THE SYNCHROTRON-DOMINATED SUPERNOVA REMNANT RX J1713.7-3946-猫眼课题宝

DOI：

10.1088/0004-637x/814/1/29

发表时间：

2015-10

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

S. Katsuda;F. Acero;N. Tominaga;Y. Fukui;J. Hiraga;K. Koyama;Shiu-Hang Lee;K. Mori;S. Nagataki;Y. Ohira;R. Petre;H. Sano;Y. Takeuchi;T. Tamagawa;N. Tsuji;H. Tsunemi;Y. Uchiyama

我们首次探测到超新星遗迹(SNR)RX J1713.7-3946的热X射线辐射，它是以同步加速器为主的小类SNR的原型。使用XMM-牛顿数据生成的柔软度比图显示，较暗的内部区域比较亮的贝壳区域更柔软。利用Suzaku和深度XMM-牛顿观测，我们从最软的区域提取了X射线光谱，在Eph∼？&gt；1和∼1.35kev发现了清晰的线特征。这些谱线可以很好地解释为来自热发射成分的Ne-Ly-α和Mg-He-α。由于热成分中金属与铁的丰度比远高于太阳值，我们将热发射归因于反向冲击的SN喷射物。太阳的Mg/Ne、Si/Ne和Fe/Ne比值分别为2.0~2.6、1.5~2.0和<0.0 5太阳，表明RX J1713.7-3946是一颗质量相对较低的恒星(≲2 0M⊙)，这与之前基于该恒星的恒星风对周围介质的影响的推断是一致的。由于∼6000km的S−1(9.6pc半径除以1600年)的平均冲击波速度比其他岩心崩塌SNR相对较快，我们认为RXJ1713.7-3946是SNIb/c的结果，其前身是相互作用双星的成员。虽然我们的分析为X射线线发射提供了强有力的证据，但我们对其性质的解释为锡喷出物的热发射需要进一步证实，特别是通过未来使用ASTRO-H进行的精密光谱测量。

We report the first detection of thermal X-ray line emission from the supernova remnant (SNR) RX J1713.7-3946, the prototype of the small class of synchrotron-dominated SNRs. A softness-ratio map generated using XMM-Newton data shows that faint interior regions are softer than bright shell regions. Using Suzaku and deep XMM-Newton observations, we have extracted X-ray spectra from the softest area, finding clear line features at E ph ∼ ?> 1 and ∼1.35 keV. These lines can be best explained as Ne Lyα and Mg Heα from a thermal emission component. Since the abundance ratios of metals to Fe are much higher than solar values in the thermal component, we attribute the thermal emission to reverse-shocked SN ejecta. The measured Mg/Ne, Si/Ne, and Fe/Ne ratios of 2.0–2.6, 1.5–2.0, and <0.05 solar suggest that the progenitor star of RX J1713.7-3946 was a relatively low-mass star (≲20 M⊙), consistent with a previous inference based on the effect of stellar winds of the progenitor star on the surrounding medium. Since the mean blastwave speed of ∼6000 km s−1 (the radius of 9.6 pc divided by the age of 1600 years) is relatively fast compared with other core-collapse SNRs, we propose that RX J1713.7-3946 is a result of an SN Ib/c whose progenitor was a member of an interacting binary. While our analysis provides strong evidence for X-ray line emission, our interpretation of its nature as thermal emission from SN ejecta requires further confirmation especially through future precision spectroscopic measurements using ASTRO-H.

EVIDENCE FOR THERMAL X-RAY LINE EMISSION FROM THE SYNCHROTRON-DOMINATED SUPERNOVA REMNANT RX J1713.7-3946

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