论文标题
我们如何解释最后的uherc各向异性？
How can we explain last UHERC anisotropies?
论文作者
论文摘要
我们考虑了UHECR（超高能量宇宙射线），聚类，组成，天空中的分布的最新结果，从几个EEV的能量（偶极偏置）到最高的EEV。自2008年以来，我们建议我们在这里重新确认，在40高达70 EEV的UHECR主要由轻质和最轻的核制成。显着的处女座缺席和少数位于附近的静脉外源，例如CENA，Ng 253，M82可以通过MPC距离内最轻的核脆性和不透明度来很好地理解。我们还评论了十个EEV的一些银河uHECR来源的作用，这可能是部分喂食螺旋杆偶极子偶极偶体的作用。最轻和重核的UHECR光谱组成的最新各向异性，外部和沿银河平面，也可能是我们先前的主张（2012年）的首次证实。较重，最有能力的UHECR银河系核与主要局部（MPC）的局部核核的相互作用似乎适合UHECR拼图的主要部分。
We consider the recent results on UHECR (Ultra High Energy Cosmic Ray), clustering, composition, distribution in the sky, from the energy of several EeV with the dipole anisotropy up to the highest ones. We have suggested since 2008 and we reconfirm here that UHECR at 40 up to 70 EeV are mostly made by light and lightest nuclei. The remarkable Virgo absence and the few localized nearby extragalactic sources as CenA, NG 253, M82 may be well understood by the lightest nuclei fragility and opacity within Mpc distances. We comment also on the role of a few galactic UHECR sources at ten EeV that may be partially feeding the Auger dipole UHECR anisotropy. The recent anisotropy in the UHECR spectral composition of lightest and heavy nuclei, outside and along the galactic plane, could also be a first confirmation of our previous claims (2012). The interplay of the heavier and most energetic UHECR galactic nuclei with the mainly local (Mpcs) extragalactic signals ruled by lightest nuclei, seems to fit the main pieces of UHECR puzzle.
