Propagation of the cosmic-ray iron group at intermediate energies

Details Propagation of the cosmic-ray iron group at intermediate energies Propagation of the cosmic-ray iron group at intermediate energies

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..96..321b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 96, no. 2, Oct. 1983, p. 321-331. Research supported by the Comision Nacio

Astronomy and Astrophysics

Astrophysics

Abundance, Astronomical Models, Cosmic Rays, Particle Energy, Energy Dissipation, Extrapolation, Interstellar Space, Iron

Scientific paper

Elemental abundances of the VH group of cosmic radiation have been measured in the energy interval 250 - 550 MeV nucl-1 in a balloon exposure at Sioux Falls (South Dakota) of a plastic detector LEXAN stack. The abundances so obtained have been extrapolated to the sources in the frame of the homogeneous model correcting for energy loss. After taking into account solar modulation, the best fit to model values has led to an escape mean free path λe = 5 E-0.4 g cm-2, where E is the energy in GeV nucl-1, for E > 1 GeV nucl-1, and a constant λe = 5 g cm-2 for E ≤ 1 GeV nucl-1. When turning to the diffusion model, also including an energy loss term, a diffusion coefficient D = 3×1028 cm2 s-1 has been estimated.

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