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

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Cited by in corpus (9)

• Bayesian analysis of cosmic-ray propagation: evidence against homogeneous diffusion
• HAWC Observations Strongly Favor Pulsar Interpretations of the Cosmic-Ray Positron Excess
• New calculation of antiproton production by cosmic ray protons and nuclei
• Constraining the origin of the rising cosmic ray positron fraction with the boron-to-carbon ratio
• Cosmic ray signatures of a 2-3 Myr old local supernova
• Measuring the Local Diffusion Coefficient with H.E.S.S. Observations of Very High-Energy Electrons
• Possible Evidence for the Stochastic Acceleration of Secondary Antiprotons by Supernova Remnants
• Pulsar interpretation of the lepton spectra measured by AMS-02
• Origin of Spectral Hardening of Secondary Cosmic-Ray Nuclei