Secondary-electron radiation accompanying hadronic GeV-TeV gamma-rays from supernova remnants
Secondary-electron radiation accompanying hadronic GeV-TeV gamma-rays from supernova remnants
复制标题
来自超新星遗迹的强子 GeV-TeV 伽马射线伴随的二次电子辐射
DOI：
10.1093/mnras/staa019
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发表时间：
2020
影响因子：
4.8
通讯作者：
Zhao Xiaohong
中科院分区：
文献类型：
--
作者：
Huang Yan;Li Zhuo;Wang Wei;Zhao Xiaohong
超新星遗迹（SNR）激波中强子相互作用产生的次级电子和正电子（SEP）的同步辐射是SNR激波中宇宙线（CR）产生的一个明显证据。在这里，我们提供了一种方法，其中所观察到的伽马射线通量从信噪比，创建π衰变，直接用于推导SEP分布，因此同步加速器光谱。我们将该方法应用到三个伽玛射线亮信噪比。在年轻的SNR RX J1713.7−3946中，如果观测到的GeV-TeV伽马射线是强子源，且SNR激波中的磁场为B 0.5 mG，则SEP可能会在10−5-10− 2 eV处产生光谱隆起，超过轻子模型预测的同步加速器分量，并在100 keV处产生软光谱拖尾，与轻子模型中的硬光谱斜率不同。在中年信噪比IC 443和W 44中，如果观测到的γ射线是强子起源的，则SEP同步辐射（B_400 -500 μG）能很好地解释观测到的射电通量和谱斜率，支持γ射线的强子起源。未来的微波到远红外和硬X射线（> 100 keV）观测被鼓励来限制SEP辐射和SNR中的伽马射线起源。
The synchrotron radiation from secondary electrons and positrons (SEPs) generated by hadronic interactions in the shock of supernova remnant (SNR) could be a distinct evidence of cosmic ray (CR) production in SNR shocks. Here, we provide a method where the observed gamma-ray flux from SNRs, created by pion decays, is directly used to derive the SEP distribution and hence the synchrotron spectrum. We apply the method to three gamma-ray bright SNRs. In the young SNR RX J1713.7−3946, if the observed GeV−TeV gamma-rays are of hadronic origin and the magnetic field in the SNR shock isB≳ 0.5 mG, the SEPs may produce a spectral bump at 10−5–10−2eV, exceeding the predicted synchrotron component of the leptonic model, and a soft spectral tail at ≳100 keV, distinct from the hard spectral slope in the leptonic model. In the middle-aged SNRs IC443 and W44, if the observed gamma-rays are of hadronic origin, the SEP synchrotron radiation withB∼ 400–500 μG can well account for the observed radio flux and spectral slopes, supporting the hadronic origin of gamma-rays. Future microwave to far-infrared and hard X-ray (>100keV) observations are encouraged to constraining the SEP radiation and the gamma-ray origin in SNRs.