论文标题
在宇宙射线上的费米气泡的可能对应信号
Possible counterpart signal of the Fermi bubbles at the cosmic-ray positrons
论文作者
论文摘要
内部银河系托管了宇宙射线爆发事件，包括负责伽马射线费米气泡的那些和X射线中的Erosita气泡。在这项工作中，我们研究了AMS-02正电子分数，并找到了12、21和48 GEV的三个功能，其中最低能量的最低能量具有1.4至4.9- $σ$的意义，具体取决于天体物理背景假设。利用背景模拟解释宇宙射线正电子的分数，正电子通量和电子以及正电子通量，由一级，次级宇宙射线和局部脉冲星的宇宙射线和宇宙射线，我们测试这些频谱特征，源自内部银河系的电子/potitron爆发事件。我们发现了12个GEV功能，可以通过年龄$τ\ simeq 3-10 $ MYR来解释；与拟议的费米气泡时代一致。此外，宇宙射线电子和沿银河盘传播的宇宙射线电子的能量估计为$ 10^{51.5} -10^{57.5} {57.5} $ ergs，或$ O（10^{ - 4}）-o（1）-o（1）-o（1）-o（1）$ COSMIC-COSMIC-ray cobuse formi cosuse formi cosuse formi cosuse formi cosuse formi cosuse formi cosuse formi cosuse formi cosuse。我们主张这些正电子分数特征，是费米气泡或其中的子结构的对应物信号，或者是Erosita气泡的信号。
The inner galaxy has hosted cosmic-ray burst events including those responsible for the gamma-ray Fermi bubbles and the eROSITA bubbles in X-rays. In this work, we study the AMS-02 positron fraction and find three features around 12, 21 and 48 GeV of which the lowest energy has a 1.4 to 4.9-$σ$ significance, depending on astrophysical background assumptions. Using background simulations that explain the cosmic-ray positron fraction, positron flux and electron plus positron flux, by primary, secondary cosmic rays and cosmic rays from local pulsars, we test these spectral features as originating from electron/positron burst events from the inner galaxy. We find the 12 GeV feature, to be explained by an event of age $τ\simeq 3 - 10$ Myr; in agreement with the proposed age of the Fermi bubbles. Furthermore, the energy in cosmic-ray electrons and positrons propagating along the galactic disk and not within the Fermi bubbles volume, is estimated to be $10^{51.5}-10^{57.5}$ ergs, or $O(10^{-4}) -O(1)$ the cosmic-ray energy causing the Fermi bubbles. We advocate that these positron fraction features, are the counterpart signals of the Fermi bubbles, or of substructures in them, or of the eROSITA bubbles.
