A scenario for second‐stage acceleration of the galactic cosmic rays beyond 1014 eV via multiple interaction with SNRs in the galactic disc is investigated. A numerical scheme taking into consideration the size frequency distribution of SNRs, the probability distribution of energy gain/loss during SNR encounter and the compositional abundances of the cosmic ray nuclei is used to illustrate the quantitative aspects of such process.

Topics
Cosmic rays, Galactic properties, Probability theory, Particle acceleration
This content is only available via PDF.
© 1992 American Institute of Physics.
1992
American Institute of Physics
You do not currently have access to this content.