Nearby source interpretation of differences among light and medium composition spectra in cosmic rays

TL;DR

This paper proposes a nearby source model to explain differences in cosmic ray spectra among light and medium-mass elements, accounting for recent precise measurements and anisotropy observations.

Contribution

It introduces a nearby source scenario with specific abundance differences to explain spectral variations and anisotropies in cosmic rays.

Findings

Nearby source abundance ratio differences explain spectral features.

The model accounts for high-energy spectral softening.

Predicted anisotropy differences below PeV energies.

Abstract

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.