10 $^{19}$ eV以上的宇宙辐射能谱的一个主要特征是重核相对于轻核的比例增加。这一事实，以及其他简单的假设，采用计算的宇宙辐射的能量谱高达2.4 $\times$ 10 $^{21}$ eV。预测的光谱保持在较低能量下观察到的指数2.67，这是银河系中加速宇宙射线的物理机制的基本、已知、经验性的良好评估特征。实际上，在10 $^{19}$ eV以上，核的注入被某些滤波器抑制，并且这种抑制导致能谱的阶梯轮廓。有人认为，粒子注入失败与能量开始与质子，其次是氦，然后由其他较重的核铀。在7.5 $\times$ 10 $^{20}$左右，宇宙辐射仅由比铜重的原子核组成，估计强度为1.8 $\times$ 10 $^{-30}$粒子/GeV s sr m $^2$。
英文摘要：
A major feature of the energy spectrum of the cosmic radiation above 10$^{19}$ eV is the increasing fraction of heavy nuclei with respect to light nuclei. This fact, along with other simple assumptions, is adopted to calculate the energy spectrum of the cosmic radiation up to 2.4$\times$10$^{21}$ eV. The predicted spectrum maintains the index of 2.67 observed at lower energies which is the basic, known, empirical well-assessed feature of the physical mechanism accelerating cosmic rays in the Galaxy. Indeed above 10$^{19}$ eV the injection of nuclei is inhibited by some filter and this inhibition causes a staircase profile of the energy spectrum. It is argued that particle injection failure versus energy commences with protons, followed by Helium and then by other heavier nuclei up to Uranium. Around 7.5$\times$10$^{20}$ the cosmic radiation consists solely of nuclei heavier than Copper and the estimated intensity is 1.8$\times$10$^{-30}$ particles/GeV s sr m$^2$.
Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理研究所）；The Pennsylvania State University（宾夕法尼亚州立大学）；Virginia Tech（弗吉尼亚理工大学）；The University of Tokyo（东京大学）
Survival of ultraheavy nuclei in astrophysical sources: applications to protomagnetar outflows
Frontier Research Institute for Interdisciplinary Sciences, Tohoku University（东北大学前沿跨学科研究院）；Astronomical Institute, Graduate School of Science, Tohoku University（东北大学理学研究科天文学研究所）；Center for Neutrino Physics, Department of Physics, Virginia Tech（弗吉尼亚理工大学物理系中微子物理中心）；Department of Physics, Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin（威斯康星大学威斯康星冰立方粒子天体物理中心物理系）；Department of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore（印度印多尔理工学院天文、天体物理与空间工程系）；Department of Physics, The Pennsylvania State University（宾夕法尼亚州立大学物理系）；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文与天体物理系）；Institute for Gravitation and the Cosmos, The Pennsylvania State University（宾夕法尼亚州立大学引力与宇宙研究所）
Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（高能物理研究所，中国科学院粒子天体物理重点实验室）；TIANFU Cosmic Ray Research Center（天府宇宙线研究中心）
