Cosmic ray electrons and positrons from supernova explosions of massive stars.
Cosmic ray electrons and positrons from supernova explosions of massive stars.
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DOI：
10.1103/physrevlett.103.061101
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发表时间：
2009-03
影响因子：
8.6
通讯作者：
P. Biermann;J. Becker;A. Meli;W. Rhode;E. Seo;T. Stanev
中科院分区：
文献类型：
--
作者：
P. Biermann;J. Becker;A. Meli;W. Rhode;E. Seo;T. Stanev
我们将最近发现的宇宙射线电子和宇宙射线正电子过量成分及其截止值归因于爆炸的沃尔夫-拉叶星和红超巨星极帽中超新星激波的加速。考虑到在这样一颗恒星周围有一个半径的球面，极帽中的磁场是径向的，而不是大部分的4 π（完整的立体角），那里的磁场几乎是切向的。这种差异产生了更平坦的光谱，也增强了宇宙射线在极帽加速的正电子注入。这一推理自然解释了观测结果。精确的光谱测量将是测试，因为它预测了一个简单的E；源中新组分的{-2}谱，陡化为E；{-3}的观测值为E；{4}。
We attribute the recently discovered cosmic ray electron and cosmic ray positron excess components and their cutoffs to the acceleration in the supernova shock in the polar cap of exploding Wolf-Rayet and red supergiant stars. Considering a spherical surface at some radius around such a star, the magnetic field is radial in the polar cap as opposed to most of 4pi (the full solid angle), where the magnetic field is nearly tangential. This difference yields a flatter spectrum, and also an enhanced positron injection for the cosmic rays accelerated in the polar cap. This reasoning naturally explains the observations. Precise spectral measurements will be the test, as this predicts a simple E;{-2} spectrum for the new components in the source, steepened to E;{-3} in observations with an E;{-4} cutoff.