Abstract

One of the unsolved problems of cosmic ray physics is determining the nature and sources of ultrahigh energy cosmic rays (UHECRs, E > 10¹⁸ eV). The high degree of isotropy of the observed UHECR intensity caused mainly by the deviations of the UHECR trajectories in extragalactic and Galactic magnetic fields, as well as the significant uncertainty in their chemical composition (atomic mass), preclude one from tracing the observed events to their sources and finding the mechanisms for their acceleration. There are two ways to reduce the influence of magnetic deflection: by considering events with extremely high energy (EHECR, E > 10²⁰ eV) and taking into account modern models of the Galactic magnetic field to correct its influence on the EHECR trajectory. In this study, the observed arrival directions of EHECRs from the Pierre Auger Observatory (PAO) and Telescope Array (TA) detectors' data are adjusted for the influence of Galactic and random extragalactic magnetic fields. New celestial positions of EHECRs are compared to the samples of potential sources used by the PAO—17 active galactic nuclei (AGNs) with powerful gamma radiation (from the 2FHL catalog) and 23 starburst galaxies (radio-flux-selected)—as well as with samples of 42 radio-galaxies from the parameterized catalog of radio-galaxies and magnetars. Taking into account the energy loss length of the nuclear component (H, He, C, Si, Fe) of EHECRs in the extragalactic environment and the expected typical distances to potential sources (~100 Mpc for H and Si-Fe and ~50 Mpc for He and C), the astrophysical objects that could be sources of relevant events were distinguished in the above samples. The potential acceleration mechanisms in the selected objects are analyzed, and the contribution of possible Galactic sources to the observed EHECR flux is evaluated.

中文翻译：

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极高能量（E> 10 20 eV）宇宙射线：潜在来源

摘要

宇宙射线物理学尚未解决的问题之一是确定超高能宇宙射线的性质和来源（UHECR，E > 10 ¹⁸ eV）。观测到的UHECR强度的高度各向同性主要是由于银河外和银河磁场中UHECR轨迹的偏离以及其化学成分（原子质量）的显着不确定性，使人无法追踪观察到的事件到它们的来源并寻找加速机制。有两种方法可以减小磁偏转的影响：通过考虑具有极高能量的事件（EHECR，E > 10 ²⁰eV），并考虑到银河磁场的现代模型来纠正其对EHECR轨迹的影响。在这项研究中，针对银河和随机河外磁场的影响，对来自皮埃尔·俄格天文台（PAO）和望远镜阵列（TA）探测器数据的EHECR的到达方向进行了调整。将EHECR的新天体位置与PAO所使用的潜在来源的样本进行比较-17个活跃的银河核（AGN）具有强大的伽马辐射（来自2FHL目录）和23个爆炸形星系（通过无线电通量选择），以及并从参数化的射电星系和磁星目录中选出42个射电星系的样本。考虑到核成分（H，He，C，Si，在河外环境中EHECRs的Fe）以及到潜在来源的预期典型距离（H和Si-Fe约为100 Mpc，He和C约为50 Mpc），在天文学家中区分了可能是相关事件来源的天体以上样品。分析了选定对象中的潜在加速机制，并评估了可能的银河源对观测到的EHECR通量的贡献。