Abstract
Solar cosmic ray propagation through the interplanetary magnetic field is considered as a random process of particles traveling along magnetic lines at a finite velocity of free motion and with a free path distributed according to an inverse power law. The propagator is presented as a sum of direct (nonscattered) flux (singular part of solution) and multiple scattered flux (regular part). In the long-time asymptotic, the regular part is described by an equation with a fractional-order derivative. Using analytical expressions for the propagator, we numerically calculate fluxes of energetic particles accelerated by shock waves generated by solar flares. The presented model is in better agreement with Ulysses and Voyager 2 data than the Perri-Zimbardo model and may therefore be recommended for use in interpreting the results of further experiments.
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