Recently the AMS-02 reported the precise measurements of the energy spectra of medium-mass compositions (Neon, Magnesium, Silicon) of primary cosmic rays, which reveal different properties from those of light compositions (Helium, Carbon, Oxygen). Here we propose a nearby source scenario, together with the background source contribution, to explain the newly measured spectra of cosmic ray Ne, Mg, Si, and particularly their differences from that of He, C, O. Their differences at high energies can be naturally accounted for by the element abundance of the nearby source. Specifically, the abundance ratio of the nearby source to the background of the Ne, Mg, Si elements is lower by a factor of ~ 1.7 than that of the He, C, O elements. Such a difference could be due to the abundance difference of the stellar evolution of the progenitor star or the acceleration process/environment, of the nearby source. This scenario can simultaneously explain the high-energy spectral softening features of cosmic ray spectra revealed recently by CREAM/NUCLEON/DAMPE, as well as the energy-dependent behaviors of the large-scale anisotropies. It is predicted that the dipole anisotropy amplitudes below PeV energies of the Ne, Mg, Si group are smaller than that of the He, C, O group, which can be tested with future measurements.

最近，AMS-02报告了对一次宇宙射线的中等质量成分（氖，镁，硅）的能谱的精确测量，这些光谱揭示了与轻成分（氦，碳，氧）不同的性质。在这里，我们提出一个附近的源情景，以及背景源的贡献，以解释新测量的宇宙射线Ne，Mg，Si的光谱，尤其是它们与He，C，O的区别。它们在高能下的区别可以是自然地由附近来源的元素丰富性造成。具体而言，附近源与Ne，Mg，Si元素本底的丰度比比He，C，O元素的丰度比低约1.7。这样的差异可能是由于邻近源的恒星恒星演化或加速过程/环境的丰度差异造成的。这种情况可以同时解释最近由CREAM / NUCLEON / DAMPE揭示的宇宙射线光谱的高能谱软化特征，以及大规模各向异性的能量依赖行为。可以预言，低于Ne，Mg，Si组的PeV能量的偶极子各向异性振幅要小于He，C，O组的PeV能量，这可以用将来的测量结果进行测试。