B/C ratio and the PAMELA positron excess

Abstract

We calculate the diffuse intensity of cosmic ray (CR) nuclei and their secondaries in the Boron-Carbon group produced by supernova remnants (SNR). The trajectories of charged particles in the SNR are modeled as a random walk in the test particle approximation. Secondary production by CRs colliding with gas in the SNR is included as a Monte Carlo process, while we use Galprop to account for the propagation and interactions of CRs in the Galaxy. In the vicinity of a source, we find an approximately constant B/C ratio as a function of energy. As a result, the B/C ratio at Earth does not rise with energy, but flattens instead in the high energy limit. This prediction can be soon tested by the AMS-2 collaboration.

4 pages, 4 eps figures, v2: one reference added

References in corpus (7)

• Observation of an anomalous positron abundance in the cosmic radiation
• A new measurement of the antiproton-to-proton flux ratio up to 100 GeV in the cosmic radiation
• The origin of the positron excess in cosmic rays
• Measurements of cosmic-ray secondary nuclei at high energies with the first flight of the CREAM balloon-borne experiment
• High-energy antiprotons from old supernova remnants
• Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei
• Antimatter spectra from a time-dependent modeling of supernova remnants