A simulation of high-energy cosmic-ray propagation

Details A simulation of high-energy cosmic-ray propagation A simulation of high-energy cosmic-ray propagation

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...319..836h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 319, Aug. 15, 1987, p. 836-841.

Other

9

Astronomical Models, Cosmic Rays, Interplanetary Magnetic Fields, Milky Way Galaxy, Plasma-Electromagnetic Interaction, Radiation Distribution, Magnetic Flux, Particle Acceleration

Scientific paper

The simulation of cosmic-ray propagation in the Galactic magnetic fields is presented in the energy region of 10 to the 16th - 10 to the 18th eV, where the gyroradius and the scale of the irregularity of the magnetic field are considered to be comparable. The diffusion tensor is calculated as a function of the ratio of the gyroradius (Rg) and the scale of the magnetic field irregularity (L0). The Rg dependence of the diffusion tensor in the region Rg greater than L0 is different from that in the region Rg less than L0. In the region Rg less than L0, the stochastic nature of the magnetic field suggested by Jokipii and Parker (1969) controls the process. In the region Rg greater than L0, like many other diffusion processes, the process can be understood in terms of the scattering centers and mean free path.

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