UHECR签名和来源

D. Fargion, P. G. De Sanctis Lucentini, M. Khlopov
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引用次数: 1

摘要

我们讨论了超高能量宇宙射线(UHECR)在天空中的聚集、组成和分布的最新结果;从偶极子各向异性中几十EeV的能量,到少数窄团的最高能量,即热点的能量。根据早期UHECR组成记录与质子的偏差,我们注意到40 EeV以上的UHECR事件不仅可以由任何轻核或重核引起,而且主要由He,D, Li, be等最轻的原子核引起。室女座的显著缺失和附近的少数星系外源,如CenA, NGC 253和M82,自然是可以理解的:最轻的UHECR核不能从室女座20 Mpc的距离到达我们,因为它们的核在几个Mpc距离以上就很脆弱。它们在宽热点上的偏转和涂抹更适合于较轻的原子核,而不是首选的质子或重核候选信使。我们注意到,即使在如此近的光源下,这些最轻的原子核仍然遭受部分光破坏。因此,在几十个EeV的多重事件链中,它们以碎片的形式被破坏,已经在近十年前被俄歇合作预料到,后来也被观察到。这些多重存在与同一个CenA NGC253源密切相关。提醒了这种相关性的统计权重。我们得出的结论是,NGC 253在较低能量的星系团的同样作用也可以在较低能量范围内提供俄歇偶极子各向异性。这种较低能量的各向异性可以被最近的Vela、Crab、LMC和Cas A贡献补充和整合。在我们目前的UHECR模型中,基于几个Mpcs局部体积中最轻的核,最近的AGN,星爆或非常接近的信噪比叠加它们的信号,冻结在不同的时代,距离和方向,产生小而宽的各向异性。建议并更新可能的测试,以确认或从替代模型中理清当前模型。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
UHECR Signatures and Sources
We discuss recent results on the clustering, composition and distribution of Ultra-High Energy Cosmic Rays (UHECR) in the sky; from the energy of several tens of EeV in the dipole anisotropy, up to the highest energy of a few narrow clusters, those of Hot Spots. Following the early UHECR composition records deviations from proton we noted that the UHECR events above 40 EeV can be made not just by any light or heavy nuclei, but mainly by the lightest ones as He,D, Li,Be. The remarkable Virgo absence and the few localized nearby extragalactic sources, such as CenA, NGC 253 and M82, are naturally understood: lightest UHECR nuclei cannot reach us from the Virgo distance of twenty Mpc, due to their nuclei fragility above a few Mpc distances. Their deflection and smearing in wide hot spots is better tuned to the lighter nuclei than to the preferred proton or heavy nuclei candidate courier. We note that these lightest nuclei still suffer of a partial photodistruction even from such close sources. Therefore, their distruption in fragments, within few tens EeV multiplet chain of events, have been expected and later on observed by Auger collaboration, nearly a decade ago. These multiplet presences, strongly correlate with the same CenA, NGC253 sources. The statistical weight of such correlation is reminded. We conclude that the same role of NGC 253 clustering at lower energies could also feed the Auger dipole anisotropy at lower energy ranges. Such lower energy anisotropy could be fed and integrated by nearest Vela, Crab, LMC and Cas A contributes. In our present UHECR model, based on lightest nuclei in local volumes of a few Mpcs, closest AGN, Star-Burst or very close SNR are superimposing their signals, frozen in different epochs, distances and directions, feeding small and wide anisotropy. Possible tests to confirm, or untangle the current model from alternative ones, are suggested and updated.
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