论文标题
klein-nishina效应和宇宙射线电子光谱
Klein-Nishina effect and the cosmic ray electron spectrum
论文作者
论文摘要
辐射能量损失在调节宇宙射线电子和/或正电子（CRE）频谱中非常重要。尤其是，反康普顿散射（ICS）的klein-nishina（kN）效应导致高能电子的效率较低，这预计将在传播的电子光谱上留下烙印。已经提出，Fermi-LAT，AMS-02和Dampe观察到的CRE光谱在50 GEV上的硬化可能是由于KN效应所致。我们在这项工作中表明，与以前的某些著作中采用的近似处理相比，从汤森制度到ICS的KN制度的过渡实际上非常顺利。结果，观察到的CRE的光谱硬化不能用kN效应来解释。这意味着需要额外的一级电子光谱。我们还提供了一个参数化形式，以在宽的能量范围内准确计算ICS损失速率。
Radiative energy losses are very important in regulating the cosmic ray electron and/or positron (CRE) spectrum during their propagation in the Milky Way. Particularly, the Klein-Nishina (KN) effect of the inverse Compton scattering (ICS) results in less efficient energy losses of high-energy electrons, which is expected to leave imprints on the propagated electron spectrum. It has been proposed that the hardening of CRE spectra around 50 GeV observed by Fermi-LAT, AMS-02, and DAMPE could be due to the KN effect. We show in this work that the transition from the Thomson regime to the KN regime of the ICS is actually quite smooth compared with the approximate treatment adopted in some previous works. As a result, the observed spectral hardening of CREs cannot be explained by the KN effect. It means that an additional hardening of the primary electrons spectrum is needed. We also provide a parameterized form for the accurate calculation of the ICS energy-loss rate in a wide energy range.
