关于GeV/TeV Cosmic Ray轻子的能谱
On the Energy Spectra of GeV/TeV Cosmic Ray Leptons
摘要：
最近从几种仪器对宇宙射线电子的观测表明，测量的电子能量分布与简单的幂律有不同程度的偏差，其形式是超过TeV能量。在100 GeV能量附近的宇宙射线正电子部分中观察到了更显著的偏差。在本文中，我们表明，所观察到的电子光谱中的过剩可以很容易地再现，而不调用任何不寻常的来源以外的宇宙射线的一般弥漫的银河系成分。所涉及的主要物理效应是Klein-Nishina抑制TeV能量附近的电子冷却速率。通过合理选择表征局域星际介质的模型参数，我们可以再现费米和HESS实验的最新观测结果。我们还发现，高正电子分数随能量增加，声称的PAMELA实验，不能解释在我们的模型与保守的模型参数。然而，我们能够重现PAMELA的结果，假设高值的星光和星际气体密度，这将是更合适的超新星遗迹附近。这个问题的一个可能的解决方案可能是，宇宙射线在它们的源附近经历了大部分的相互作用，这是由于在超新星激波的远上游，自我生成的宇宙射线驱动的湍流有效地捕获了它们。
英文摘要：
Recent observations of cosmic ray electrons from several instruments have revealed various degrees of deviation in the measured electron energy distribution from a simple power-law, in a form of an excess around TeV energies. An even more prominent deviation has been observed in the fraction of cosmic ray positrons around 100 GeV energies. In this paper we show that the observed excesses in the electron spectrum may be easily re-produced without invoking any unusual sources other than the general diffuse Galactic components of cosmic rays. The primary physical effect involved is the Klein-Nishina suppression of the electron cooling rate around TeV energies. With a very reasonable choice of the model parameters characterizing the local interstellar medium, we can reproduce the most recent observations by Fermi and HESS experiments. We also find that high positron fraction increasing with energy, as claimed by the PAMELA experiment, cannot be explained in our model with the conservative set of the model parameters. We are able, however, to reproduce the PAMELA results assuming high values of the starlight and interstellar gas densities, which would be more appropriate for vicinities of supernova remnants. A possible solution to this problem may be that cosmic rays undergo most of their interactions near their sources due to the efficient trapping in the far upstream of supernova shocks by self-generated, cosmic ray-driven turbulence.
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