# Simulations of cosmic-ray particle diffusion

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## Abstract

The diffusion of charged particles in a stochastic magnetic field (strength*B*′) which is superimposed on a uniform magnetic field*B*_{0}**k** is studied. A slab model of the stochastic magnetic field is used. Many particles were released into different realizations of the magnetic field and their subsequent displacements Δ*z* in the direction of the uniform magnetic field numerically computed. The particle trajectories were calculated over periods of many particle scattering times. The ensemble average\(\left\langle {\left( {\Delta z} \right)^2 } \right\rangle \) was then used to find the parallel diffusion coefficient\(\left( {{\text{i}}{\text{.e}}{\text{.,}}K_\parallel = {{\frac{1}{2}\left\langle {\left( {\Delta z} \right)2} \right\rangle } \mathord{\left/ {\vphantom {{\frac{1}{2}\left\langle {\left( {\Delta z} \right)2} \right\rangle } {\Delta t}}} \right. \kern-\nulldelimiterspace} {\Delta t}}} \right)\). The simulations were performed for several types of stochastic magnetic fields and for a wide range of particle gyro-radius and the parameter*B′/B*_{0}. The calculations have shown that the theory of charged particle diffusion is a good approximation even when the stochastic magnetic field is of the same strength as the uniform magnetic field.

### Keywords

Magnetic Field Diffusion Coefficient Charged Particle Particle Trajectory Uniform Magnetic Field## Preview

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### References

- Urch, I. H.: 1984, to be published.Google Scholar