The Gamma-Ray Emission from the Supernova Remnant RX J1713.7-3946 Interacting with Two-phase Medium
The Gamma-Ray Emission from the Supernova Remnant RX J1713.7-3946 Interacting with Two-phase Medium
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DOI：
10.3847/1538-4357/ac731e
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发表时间：
2022-05
期刊：
影响因子：
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通讯作者：
Y. Fujita;R. Yamazaki;Y. Ohira
中科院分区：
文献类型：
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作者：
Y. Fujita;R. Yamazaki;Y. Ohira
我们研究了超新星遗迹（SNR）RX J1713.7-3946的伽马射线的起源。使用一个分析模型，我们计算宇宙射线（CR）周围的SNR的分布。受前人研究结果的启发，我们假设SNR与两相星际介质（ISM）相互作用，其中致密的团块被纤细的团块间介质包围。我们还假设，只有更高能量的质子（100 TeV）可以穿透致密的团块。我们发现质子产生的π 0衰变γ射线再现了观测到的γ射线谱，峰值在2.5TeV。另一方面，最近已经表明，在横跨SNR的网格点处观测到的ISM柱密度（NP）、X射线表面亮度（IX）和伽马射线表面亮度（Ig）在三维（3D）空间（NP，IX，Ig）中形成平面。我们发现，如果ISM或CR的电子质子比不是球形均匀的，平面配置是自然再现。我们表明，在3D空间中的观测数据的移位可以用来确定哪些数量，ISM密度，CR电子质子比，或磁场，在SNR的方位角方向上变化。
We study the origin of gamma-rays from the supernova remnant (SNR) RX J1713.7-3946. Using an analytical model, we calculate the distribution of cosmic rays (CRs) around the SNRs. Motivated by the results of previous studies, we assume that the SNR is interacting with two-phase interstellar medium (ISM), where dense clumps are surrounded by tenuous interclump medium. We also assume that only higher-energy protons (≳TeV) can penetrate the dense clumps. We find that π 0-decay gamma-rays produced by protons reproduce the observed gamma-ray spectrum peaked at ∼TeV. On the other hand, it has recently been indicated that the observed ISM column density (N p ), the X-ray surface brightness (I X ), and the gamma-ray surface brightness (I g ) at grid points across the SNR form a plane in the three-dimensional (3D) space of (N p , I X , I g ). We find that the planar configuration is naturally reproduced if the ISM or the CR electron-to-proton ratio is not spherically uniform. We show that the shift of the observed data in the 3D space could be used to identify which of the quantities, the ISM density, the CR electron-to-proton ratio, or the magnetic field, varies in the azimuthal direction of the SNR.