论文标题
鉴于最近观察到的逆孔孔光环
Contribution of pulsars to cosmic-ray positrons in light of recent observation of inverse-Compton halos
论文作者
论文摘要
在观察到$γ$ ray的$γ$ ray排放量之后，在Geminga和Monogem Pwne周围的几个程度尺寸的Tev Energies，在Geminga的Geminga afe Geminga上，在Tev Energies的Tev Energies a $γ$ - 射击能量时，已经巩固了脉冲星风（pwne）可以显着促进过多的宇宙宇宙通量（$ e^+$）宇宙及时通量的假说。这些闪烁岩周围的$γ$ ray光晕被解释为由于电子（$ e^ - $）和$ e^+$被其旋转和逃脱的$ e^+$，而compton compton散射散射的星际辐射场低能光子。这些光环的延伸表明，相对于星系中的平均值，围绕这些石的扩散抑制了两个数量级。我们实施了一个两区扩散模型，以通过pwne的银河种群加速$ e^+$的传播。我们考虑来自ATNF目录中的脉冲星，并建立对PWN银河种群的模拟。在这两种情况下，我们都会发现，在两个区域扩散模型中，pwne和Secondary $ e^+$的总贡献位于AMS-02数据的级别，以效率pulsar旋转能量$ e^\ pm的$ e^\ pm $ of $η\ sim0.1 $。对于模拟的怪胎，确定了一个$1σ$的不确定性频段，它至少是一个数量级，从10 GEV到几个TEV。即使它与每个源周围的低扩散气泡的半径相连接，也发现了Tev Energies下减少$ E^+$通量的提示。
The hypothesis that pulsar wind nebulae (PWNe) can significantly contribute to the excess of the positron ($e^+$) cosmic-ray flux has been consolidated after the observation of a $γ$-ray emission at TeV energies of a few degree size around Geminga and Monogem PWNe, and at GeV energies for Geminga at a much larger extension. The $γ$-ray halos around these PWNe are interpreted as due to electrons ($e^-$) and $e^+$ accelerated and escaped by their PWNe, and inverse Compton scattering low-energy photons of the interstellar radiation fields. The extension of these halos suggests that the diffusion around these PWNe is suppressed by two orders of magnitude with respect to the average in the Galaxy. We implement a two-zone diffusion model for the propagation of $e^+$ accelerated by the Galactic population of PWNe. We consider pulsars from the ATNF catalog and build up simulations of the PWN Galactic population. In both scenarios, we find that within a two-zone diffusion model, the total contribution from PWNe and secondary $e^+$ is at the level of AMS-02 data, for an efficiency of conversion of the pulsar spin down energy in $e^\pm$ of $η\sim0.1$. For the simulated PWNe, a $1σ$ uncertainty band is determined, which is of at least one order of magnitude from 10 GeV up to few TeV. The hint for a decreasing $e^+$ flux at TeV energies is found, even if it is strongly connected to the chosen value of the radius of the low diffusion bubble around each source.
