宇宙射线在其加速器附近的超扩散及由此产生的γ射线发射
Superdiffusion of cosmic rays in the vicinity of their accelerators and the resulting $γ$-ray emission
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中文总结 AI 辅助
研究宇宙射线在加速器附近的分布，考虑超扩散情况，分析其对射线分布的影响，包括脉冲和稳态注入时的不同表现，还计算了γ射线发射，发现可通过γ射线形态区分超扩散与正常扩散。
中文摘要 AI 辅助
我们研究宇宙射线（CRs）在其加速器附近的分布，假设在加速器周围星际介质中CRs的传输由超扩散描述，而非正常扩散。我们发现，以超扩散参数α为特征的超扩散率对CRs分布有显著影响。对于脉冲注入，CR分布呈现恒定径向分布，在距加速器大距离r处，α<2时有幂律尾，α = 2时有高斯尾。对于稳态注入，CR质子的径向分布趋于与r^(α - 3)成比例，而CR电子由于严重能量损失，其径向分布可能偏离r^(α - 3)。我们还计算了加速器周围100 pc区域内CRs与周围气体和辐射场相互作用产生的γ射线发射。我们发现，通过研究γ射线形态，利用当前和下一代成像空气切伦科夫望远镜可区分超扩散与正常扩散。
英文摘要
We study the distribution of cosmic rays (CRs) in the vicinity of their accelerators, assuming that the transport of CRs in the interstellar medium surrounding the accelerators is described by the superdiffusion, beyond the normal diffusion. We find that the superdiffusivity, which is characterized by the superdiffusion parameter $α$, impacts significantly the distribution of CRs. For impulsive injection, the CR distribution behaves a constant radial profile, except with a power-law tail for $α< 2$ or a Gaussian tail for $α=2$ at large distance, $r$, from the accelerators. For stationary injection, the radial profile of CR protons tends to being proportional to $r^{α- 3}$, while that of CR electrons can deviate from the $r^{α- 3}$ profile, due to their severe energy losses. We also compute the $γ$-ray emission, produced by the interactions of CRs with ambient gas and radiation fields, within 100 pc regions around the accelerators. We find that by investigating the $γ$-ray morphology, we can distinguish the superdiffusion from the normal diffusion with present and next-generation imaging air Cherenkov telescopes.
