Advertisement

Space Science Reviews

, Volume 99, Issue 1–4, pp 85–94 | Cite as

The Energy Spectra and Anisotropies of Cosmic Rays

  • S.P. Swordy
Article

Abstract

The existing paradigm of the origin of Galactic cosmic rays places strong supernovae shocks as the acceleration site for this material. However, although the EGRET gamma-ray telescope has reported evidence for GeV gamma rays from some supernovae, it is still unclear if the signal is produced by locally intense cosmic rays. Although non-thermal X-ray emissions have been detected from supernova remnants and interpreted as synchrotron emission from locally intense electrons at energies up to ∼100 TeV, the inferred source energy spectral slopes seem much steeper than the electron source spectrum observed through direct measurements. It remains the case that simple energetics provide the most convincing argument that supernovae power the bulk of cosmic rays. Two characteristics which can be used to investigate this issue at high energy are the source energy spectra and the source composition derived from direct measurements.

Keywords

Energy Spectrum Electron Source Supernova Remnant Source Spectrum Spectral Slope 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Asakimori, K. et al.: 1998, Astrophys. J. 502, 278.Google Scholar
  2. Axford, W. I.: 1981, Proc. 17th Int. Cosmic Ray. Conf. 12, 155.Google Scholar
  3. Binns, W. R. et al.: 1988, Astrophys. J. 324, 1106.Google Scholar
  4. Clay, R. W. et al.: 1997, Proc. 25th Int. Cosmic Ray Conf. 4, 185.Google Scholar
  5. Cronin, J. W., Gaisser, T. K., and Swordy, S. P.: 1997, ‘Cosmic Rays at Energy Frontier’, Scientific American, January issue.Google Scholar
  6. Engelmann, J. J. et al.: 1990, Astron. Astrophys. 233, 96.Google Scholar
  7. Ichimura, M. et al.: 1993, Phys. Rev. D48, 1949.Google Scholar
  8. Juliusson, E. and Meyer, J.-P.: 1973, Astrophys. Lett. 14, 153.Google Scholar
  9. Meyer, J.-P.: 1985, Astrophys. J. Suppl. 57, 173.Google Scholar
  10. Meyer, J.-P. et al.: 1997, Astrophys. J. 487, 182.Google Scholar
  11. Muller, D. et al.: 1991, Astrophys. J. 374, 356.Google Scholar
  12. Reames, D. V.: 1995, Adv. Space. Res. 15, 41.Google Scholar
  13. Seo, E. S. and Ptuskin, V. S.: 1994, Astrophys. J. 431, 705.Google Scholar
  14. Seo, E. S. et al.: 1991, Astrophys. J. 378, 763.Google Scholar
  15. Smith, L. H. et al.: 1973, Astrophys. J. 180, 987.Google Scholar
  16. Swordy, S. P.: 1995, Proc 24th Int. Cosmic Ray Conf. 2, 697.Google Scholar
  17. Swordy, S. P. et al.: 1990, Astrophys. J. 349, 625.Google Scholar
  18. Swordy, S. P. et al.: 1993, Proc. 23rd Int. Cosmic Ray Conf., Invited and Rapp. 243.Google Scholar

Copyright information

© Kluwer Academic Publishers 2001

Authors and Affiliations

  • S.P. Swordy
    • 1
  1. 1.Enrico Fermi Institute and Department of PhysicsUniversity of ChicagoU.S.A

Personalised recommendations