ESCAPE OF COSMIC-RAY ELECTRONS FROM SUPERNOVA REMNANTS
ESCAPE OF COSMIC-RAY ELECTRONS FROM SUPERNOVA REMNANTS
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DOI：
10.1111/j.1365-2966.2012.21908.x
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发表时间：
2011-06
影响因子：
4.8
通讯作者：
Y. Ohira;R. Yamazaki;N. Kawanaka;K. Ioka
中科院分区：
文献类型：
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作者：
Y. Ohira;R. Yamazaki;N. Kawanaka;K. Ioka
我们研究了宇宙射线（CR）电子从超新星遗迹（SNR）向星际空间的逃逸。结果表明，CR电子从高能量到低能逃逸，其光谱与CR核相似，但逃逸开始晚于Sedov相的开始，信噪比为1−7×10 3年，CR电子逃逸的最大能量在膝盖以下，约为0.3−50 TeV，这是因为与CR核不同，CR电子由于同步辐射而失去能量。最高能量的CR电子将被AMS-02， CALET， CTA和LHAASO实验直接探测到，或者已经被H.E.S.S.作为光谱截止点探测到。此外，我们还计算了失控CR电子在信噪比周围的空间分布及其辐射谱。与普遍看法相反，同步辐射的最大能量光子约为1 keV，是由SNR内失控的CR电子发射的。失控CR电子的逆康普顿散射可以通过介子衰变控制失控CR核的伽马射线发射，CTA和LHAASO可以检测到这两种散射，作为CR起源和信噪比周围磁波动放大的线索。我们还讨论了中年和/或老信噪比作为未识别的高能伽玛射线源。主题标题：粒子加速-宇宙射线-伽马射线：ISM - ISM：超新星遗迹-冲击波-辐射机制：非热
We investigate the escape of cosmic ray (CR) electrons from a supernova remnant (SNR) to the interstellar space. We show that CR electrons escape in order from high to low energy with a similar spectrum to CR nuclei, while the escape starts later than the beginning of the Sedov phase at an SNR age of 1−7×10 3 yrs and the maximum energy of runaway CR electrons is below the knee about 0.3− 50 TeV because unlike CR nuclei, CR electrons lose their energy due to synchrotron radiation. Highest energy CR electrons will be directly probed by AMS-02, CALET, CTA and LHAASO experiments, or have been already detected by H.E.S.S. as the spectral cutoff. Furthermore, we also calculate the spatial distribution of runaway CR electrons and their radiation spectra around SNRs. Contrary to common belief, maximum-energy photons of synchrotron radiation around 1 keV are emitted by runaway CR electrons inside the SNR. Inverse Compton scattering by runaway CR electrons can dominate the gamma-ray emission from runaway CR nuclei via pion decay, and both are detectable by CTA and LHAASO as clues to the CR origin and the amplification of magnetic fluctuations around the SNR. We also discuss middle-aged and/or old SNRs as unidentified very-high-energy gamma-ray sources. Subject headings: acceleration of particles — cosmic rays — gamma rays: ISM — ISM: supernova remnants — shock waves — radiation mechanisms: non-thermal