TL;DR
This paper models how supernova remnants accelerate cosmic rays, explaining the observed spectral features and proposing a division of Galactic cosmic rays into two populations based on energy and release timing.
Contribution
It extends the Chevalier self-similar solution to show how supernova remnants produce two distinct cosmic ray populations with different energies and release mechanisms.
Findings
High-energy CRs (>200 GeV) are released upstream during acceleration.
Lower-energy CRs (<200 GeV) are advected into SNR and released later.
The spectral index change in Galactic CRs may correspond to this division.
Abstract
We extend the self-similar solution derived by Chevalier for a Sedov blast wave accelerating cosmic rays (CR) to show that the Galactic CR population can be divided into: (A) CR with energies above ~200GeV released upstream during CR acceleration by supernova remnants (SNR), (B) CR advected into the interior of the SNR during expansion and then released from the SNR at the end of its life to provide the Galactic CR component below ~200GeV. The intersection between the two populations may correspond to a measured change in the Galactic CR spectral index at this energy.
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