Hostname: page-component-7b7567c8c-2n9c9 Total loading time: 0 Render date: 2026-11-15T16:39:38.217Z Has data issue: false hasContentIssue false
  • English
  • Français

Interpretation of Cosmic Ray Composition: the Pathlength Distribution

Published online by Cambridge University Press:  14 August 2015

R. J. Protheroe and
J. F. Ormes
R. J. Protheroe
Affiliation:
Laboratory for High Energy Astrophysics NASA/Goddard Space Flight Center, Greenbelt, MD, U.S.A.G.M. Comstock Cosmo-Science Associates, Stony Brook, NY, USA
J. F. Ormes
Affiliation:
Laboratory for High Energy Astrophysics NASA/Goddard Space Flight Center, Greenbelt, MD, U.S.A.G.M. Comstock Cosmo-Science Associates, Stony Brook, NY, USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the 'Save PDF' action button.

The chemical composition of cosmic ray nuclei with 3≤Z≤28 between ~100 MeV/nuc and a few hundred GeV/nuc are compared with a consistent set of propagation calculations. These include the effects of spallation (energy-dependent cross sections are used), escape and ionization loss in the interstellar medium and deceleration in the solar cavity. This has enabled a consistent study of the cosmic ray pathlength distribution to be made over this entire energy range. Details of the propagation calculation are left to a forthcoming paper.

Information

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 94: Origin of Cosmic Rays , 1981, pp. 107 - 108
Copyright
Copyright © Reidel 1981 

References

Benegas, J.C., et al., 1975: Proc. Munich Conf. 1, 251.Google Scholar
Cowsik, R., and Wilson, L.W., 1973: Proc. Denver Conf. 1, 500.Google Scholar
Cowsik, R., and Wilson, L.W., 1975: Proc. Munich Conf. 2, 659.Google Scholar
Freier, P.S. et al., 1979: Proc. Kyoto Conf. 1, 316.Google Scholar
Garcia-Munoz, M., et al., 1977: Proc. Plovdiv Conf. 1, 224.Google Scholar
Garcia-Munoz, M., et al., 1979: Proc. Kyoto Conf. 1, 310.Google Scholar
Israel, M.H., et al., 1979: Proc. Kyoto Conf. 1, 232 and 13, 402.Google Scholar
Koch, L., 1980: Bull. A.P.S. 25, 563.Google Scholar
Lezniak, J.A., and Webber, W.R., 1978: Astrophys. Space Sci. 63, 35.CrossRefGoogle Scholar
Lund, N., et al., 1975: Proc. Munich Conf. 1, 263.Google Scholar
Maehl, R.C., et al., 1977: Astrophys. Space Sci. 47, 163.CrossRefGoogle Scholar
Ormes, J.F., and Freier, P.S., 1978: Astrophys. J. 222, 471.CrossRefGoogle Scholar
Scarlett, W.R., et al., 1978: Astrophys. Space Sci. 59, 301.CrossRefGoogle Scholar
Shapiro, M.M., et al., 1973: Proc. Denver Conf. 1, 578.Google Scholar
Simon, M., 1977: Astron. Astrophys. 61, 833.Google Scholar