A possible correlation between the high energy electron spectrum and the   cosmic-ray secondary-to-primary ratios
  Recent observations of high energy cosmic-ray electrons by the Fermi-LAT and the HESS experiments between $20$ GeV and $5$ TeV have found that the energy spectrum closely follow a broken power-law with a break at around $1$ TeV. On the other hand, measurements of cosmic-ray secondary-to-primary ratios like the boron-to-carbon ratio seem to indicate a possible change in the slope at energies around $100$ GeV/n. In this paper, we discuss one possible explanation for the observed break in the electron spectrum and its possible correlation with the flattening in the secondary-to-primary ratios at higher energies. In our model, we assume that cosmic-rays after acceleration by supernova remnant shock waves, escape downstream of the shock and remain confined within the remnant until the shock slows down. During this time, the high-energy electrons suffer from radiative energy losses and the cosmic-ray nuclei undergo nuclear fragmentations due to their interactions with the matter. Once the cosmic-rays are released from the supernova remnants, they follow diffusive propagation in the Galaxy where they further suffer from radiative or fragmentation losses. 
Satyendra Thoudam (Nijmegen) and J\"org R. H\"orandel (Nijmegen)
astro-ph.HE