论文标题
Pulsar Halos罕见吗？
Are pulsar halos rare ?
论文作者
论文摘要
扩展的伽马射线发射被解释为通过电子 - 峰值对环境光子的逆孔子散射形成的光晕，朝向许多中年脉冲星。银河系中现象的物理起源和实际共同点尚不清楚。与最近的理论模型中可以实现的相比，配对限制的条件似乎很极端。我们搜索了最小化J0633+1746和B0656+14中光环中扩散抑制的程度和幅度的场景，如果将它们应用于附近的所有附近的中年脉冲脉冲，则探索了对局部正电子通量的含义。我们使用了现象学静态的两区扩散框架，并将其预测与Fermi-LAT和HAWC观察结果进行了比较，并与AMS-02测量的局部正电子通量进行了比较。尽管数据需要在〜100TEV处的2-3个数量级的强扩散抑制，但可以找到两个物体的扩散抑制扩散剂量较小至30％的溶液。如果附近的所有中年脉冲星形成了这样的光晕，则它们的共同正常通量（包括Geminga的贡献）将使> 100GEV AMS-02测量的注射效率测量，这些效率比J0633+1746和B0656和B0656和B0656+14中的规范晕圈的注射效率要小得多，并具有典型的典型的puls。 Conversely, if positrons from other nearby pulsars are released in the interstellar medium without any confinement around the source, their total positron flux fits into the observed spectrum for the same injection efficiencies of a few tens of percent for all pulsars, from kyr-old objects powering pulsar wind nebulae to 100kyr-old objects like J0633+1746 and B0656+14.假设大多数中年脉冲星未产生光环（删节）似乎是一个简单的情况。
Extended gamma-ray emission, interpreted as halos formed by the inverse-Compton scattering of ambient photons by electron-positron pairs, is observed toward a number of middle-aged pulsars. The physical origin and actual commonness of the phenomenon in the Galaxy remain unclear. The conditions of pair confinement seem extreme compared to what can be achieved in recent theoretical models. We searched for scenarios minimizing as much as possible the extent and magnitude of diffusion suppression in the halos in J0633+1746 and B0656+14, and explored the implications on the local positron flux if they are applied to all nearby middle-aged pulsars. We used a phenomenological static two-zone diffusion framework and compared its predictions with Fermi-LAT and HAWC observations of the two halos, and with the local positron flux measured with AMS-02. While strong diffusion suppression by 2-3 orders of magnitude at ~100TeV is required by the data, it is possible to find solutions with diffusion suppression extents as small as 30pc for both objects. If all nearby middle-aged pulsars develop such halos, their combined positron flux including the contribution from Geminga would saturate the >100GeV AMS-02 measurement for injection efficiencies that are much smaller than those inferred for the canonical halos in J0633+1746 and B0656+14, and more generally with the values typical of younger pulsar wind nebulae. Conversely, if positrons from other nearby pulsars are released in the interstellar medium without any confinement around the source, their total positron flux fits into the observed spectrum for the same injection efficiencies of a few tens of percent for all pulsars, from kyr-old objects powering pulsar wind nebulae to 100kyr-old objects like J0633+1746 and B0656+14. It seems a simpler scenario to assume that most middle-aged pulsars do not develop halos (abridged).
