论文标题
脉冲星在宇宙射线电子和正电子光谱中不会产生鲜明的特征
Pulsars Do Not Produce Sharp Features in the Cosmic-Ray Electron and Positron Spectra
论文作者
论文摘要
脉冲星被认为是Pamela和AMS-02检测到的宇宙射线上的过量的主要解释。标准脉冲星模型的一个显着特征是通过同步加速器和逆孔普通工艺对非常高能电子的效率越来越有效冷却产生的急剧光谱截止。这种光谱中断已被用于：（1）约束导致多余的脉冲星的年龄，（2）认为大量脉冲星必须显着促进正电子通量，并且（3）认为光谱截止不能区分暗物质和脉冲星模型。我们证明了这种光谱特征不存在 - 它似乎是由于将反相对散射视为连续的近似值而不是离散和灾难性的，能量损害的过程。天体物理来源不会通过冷却来产生鲜明的光谱特征，从而重新开放了这种特征会为暗物质提供无可争议的证据的可能性。
Pulsars are considered to be the leading explanation for the excess in cosmic-ray positrons detected by PAMELA and AMS-02. A notable feature of standard pulsar models is the sharp spectral cutoff produced by the increasingly efficient cooling of very-high-energy electrons by synchrotron and inverse-Compton processes. This spectral break has been employed to: (1) constrain the age of pulsars that contribute to the excess, (2) argue that a large number of pulsars must significantly contribute to the positron flux, and (3) argue that spectral cutoffs cannot distinguish between dark matter and pulsar models. We prove that this spectral feature does not exist -- it appears due to approximations that treat inverse-Compton scattering as a continuous, instead of as a discrete and catastrophic, energy-loss process. Astrophysical sources do not produce sharp spectral features via cooling, reopening the possibility that such a feature would provide incontrovertible evidence for dark matter.
