UHE质子在磁化宇宙网中的传输
Propagation of UHE Protons through Magnetized Cosmic Web
摘要：
如果超高能宇宙射线（UHECR）起源于河外源，那么了解带电粒子在宇宙磁化大尺度结构（LSS）中的传播对于寻找天体物理加速器至关重要。基于一种新的湍流发电机模型，我们估计了LSS形成的宇宙学模拟中的星系际磁场（IGMF）。在UHECR源与LSS强相关的前提下，我们考虑一个模型，其中E >10^{19} eV的质子由代表位于星系团内部的活动星系核的源注入。利用IGMF模型，我们跟踪质子的轨迹，同时考虑到由于与宇宙背景辐射相互作用而导致的能量损失。对于位于像我们这样的星系群内部的观测者来说，大约70%和35%的60 EeV以上的UHECR事件分别到达源位置的~15度和~5度范围内，时间延迟小于~10^7年。这意味着超GZK质子的到达方向可能与天空中宇宙学源的分布相关。在这个模型中，附近的源（在10 - 20 Mpc内）应该对~10^{20} eV以上的粒子通量有显著的贡献。
英文摘要：
If ultra-high-energy cosmic rays (UHECRs) originate from extragalactic sources, understanding the propagation of charged particles through the magnetized large scale structure (LSS) of the universe is crucial in the search for the astrophysical accelerators. Based on a novel model of the turbulence dynamo, we estimate the intergalactic magnetic fields (IGMFs) in cosmological simulations of the formation of the LSS. Under the premise that the sources of UHECRs are strongly associated with the LSS, we consider a model in which protons with E >10^{19} eV are injected by sources that represent active galactic nuclei located inside clusters of galaxies. With the model IGMFs, we then follow the trajectories of the protons, while taking into account the energy losses due to interactions with the cosmic background radiation. For observers located inside groups of galaxies like ours, about 70% and 35% of UHECR events above 60 EeV arrive within ~15 degree and ~5 degree, respectively, of the source position with time delays of less than ~10^7 yr. This implies that the arrival direction of super-GZK protons might exhibit a correlation with the distribution of cosmological sources on the sky. In this model, nearby sources (within 10 - 20 Mpc) should contribute significantly to the particle flux above ~10^{20} eV.
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