Signatures of the Origin of High-Energy Cosmic Rays in Cosmological Gamma-Ray Bursts
Signatures of the Origin of High-Energy Cosmic Rays in Cosmological Gamma-Ray Bursts
复制标题
宇宙伽马射线暴中高能宇宙射线起源的特征
DOI：
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发表时间：
1996
期刊：
影响因子：
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通讯作者：
E. Waxman
中科院分区：
文献类型：
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作者：
J. Miralda;E. Waxman
我们得到的假设，宇宙射线（CR）的能量大于1019 eV的起源于相同的宇宙学对象产生伽马射线暴（GRBs）的观测结果。在这个模型中，需要10-12 G的星系际磁场，以便通过在CR到达时间中产生能量依赖的延迟来连续地观测CR。这导致各个CR源具有非常窄的观测光谱，因为在任何给定时间，仅观测到具有固定时间延迟的那些CR。因此，最亮的CR源在不同的能量下应该是不同的。贡献于总CR通量的源的平均数随着能量的减少比稳定CR源的模型快得多，在Ecrit = 1020 × 1020 eV时下降到1，对星系际磁场强度的敏感性非常弱。在Ecrit以下，预计会有大量的源，与观测结果一致。在E临界以上，如果附近最近发生了伽玛暴，则可以观察到一个源的通量大大高于所有源的时间平均CR通量。如果存在这样的源，其狭窄的光谱可能会在总光谱中产生“间隙”。这些特征应该可以通过计划的“俄歇”CR实验检测到。
We derive observational consequences for the hypothesis that cosmic rays (CRs) of energy greater than 1019 eV originate in the same cosmological objects producing gamma-ray bursts (GRBs). Intergalactic magnetic fields ≳10-12 G are required in this model to allow CRs to be observed continuously in time by producing energy-dependent delays in the CR arrival times. This results in individual CR sources having very narrow observed spectra, since at any given time only those CRs having a fixed time delay are observed. Thus, the brightest CR sources should be different at different energies. The average number of sources contributing to the total CR flux decreases with energy much more rapidly than in a model of steady CR sources, dropping to one at Ecrit ≃ 2 × 1020 eV with very weak sensitivity to the intergalactic magnetic field strength. Below Ecrit, a very large number of sources is expected, consistent with observations. Above Ecrit, a source may be observed with a flux considerably higher than the time-averaged CR flux from all sources, if a nearby GRB occurred recently. If such a source is present, its narrow spectrum may produce a “gap” in the total spectrum. These signatures should be detectable by the planned “Auger” CR experiment.