Sources of primary cosmic rays forming the bump near E0=100 PeV

TL;DR

This paper investigates the irregularities in the primary cosmic rays spectrum near 100 PeV by analyzing the relationship between variable star types and cosmic ray energies, revealing stellar contributions to spectral features.

Contribution

It establishes a link between variable star periods and the maximum energy of cosmic ray nuclei, explaining spectral irregularities through stellar type transitions.

Findings

The knee at 3-5 PeV is linked to a decrease in SRB stars and an increase in Mira stars.

The 80 PeV bump is formed by giant and super-giant Mira and SRC stars.

Spectral irregularities are associated with transitions between dominant star types.

Abstract

The comparative primary cosmic rays (PCR) comparative analysis by E0 and the spectra of variable stars by periods is carried out in order to establish the causes of irregularities in the spectrum of PCR by E0. The relationship between the periods of variable stars and the maximum energy E0 of the nuclei of PCRs generated by these types of stars is shown. Irregularities in the PCR spectrum by E0 are associated with the transition from one dominant stars type to another. The knee in the PCR spectrum at E0 = 3-5 PeV is associated with a decrease in the contribution of SRB variability stars and a further increase in the contribution of Mira variable stars to the PCR flux. The bump in the PCR spectrum with a maximum at E0 = 80 PeV is formed by giant stars and super-giants of the Mira and SRC variability.