Cosmic-ray propagation in the Galaxy and in the heliosphere - The path-length distribution at low energy

Details Cosmic-ray propagation in the Galaxy and in the heliosphere - The path-length distribution at low energy Cosmic-ray propagation in the Galaxy and in the heliosphere - The path-length distribution at low energy

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apjs...64..269g&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 64, May 1987, p. 269-304. Research supported by Louisiana State U

Astronomy and Astrophysics

Astrophysics

133

Cosmic Rays, Particle Energy, Radiation Distribution, Wave Propagation, Abundance, Energy Spectra, Mean Free Path, Primary Cosmic Rays, Secondary Cosmic Rays

Scientific paper

The energy dependence of the path-length distribution of cosmic rays at low energies, below relativistic velocities, is studied, and its implications for models of cosmic-ray confinement and propagation in the Galaxy and Galactic halo, including the effects of a possible Galactic wind, are studied. It is found that the mean free path in Galactic propagation must be fully energy-dependent, with the mean of an exponential path-length distribution increasing with increasing energy below 1 GeV per nucleon and decreasing with increasing energy above 1 GeV per nucleon. This indicates that, at low energies, diffusion is not the controlling process. The path-length distribution is not purely exponential but is depleted in short path lengths at low energies. This depletion is energy-dependent, being largest at low energies and decreasing with increasing energy.

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