  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
$\sim1.7$ 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.
