Cosmic-Ray Nuclei, Antiprotons and Gamma-rays in the Galaxy: a New Diffusion Model

Jul, 2008
17 pages
Published in:
  • JCAP 10 (2008) 018,
  • JCAP 04 (2016) E01 (erratum)
e-Print:

Citations per year

20082012201620202024010203040
Abstract: (arXiv)
We model the transport of cosmic ray nuclei in the Galaxy by means of a new numerical code. Differently from previous numerical models we account for a generic spatial distribution of the diffusion coefficient. We found that in the case of radially uniform diffusion, the main secondary/primary ratios (B/C, N/O and sub-Fe/Fe) and the modulated antiproton spectrum match consistently the available observations. Convection and re-acceleration do not seem to be required in the energy range we consider: 1E1031 \le E \le 10^3 GeV/nucleon. We generalize these results accounting for radial dependence of the diffusion coefficient, which is assumed to trace that of supernova remnants. While this does not affect the prediction of secondary/primary ratios, the simulated longitude profile of the diffuse γ\gamma-ray emission is significantly different from the uniform case and may agree with EGRET measurements without invoking {\it ad hoc} assumptions on the galactic gas density distribution.
  • anti-p: cosmic radiation
  • nucleus: cosmic radiation
  • diffusion: model
  • space dependence
  • gamma ray: cosmic radiation
  • galaxy
  • interpretation of experiments