A Monte Carlo simulation of magnetic field line tracing in the solar wind

It is well known that the structure of magnetic field Lines in solar wind c an be influenced by the presence of the magnetohydrodynamic turbulence. We have developed a Monte Carlo simulation which traces the magnetic field lin es in the heliosphere, including the effects of magnetic turbulence. These effects are modeled by random operators which are proportional to the squar e root of the magnetic field Line diffusion coefficient. The modeling of th e random terms is explained, in detail, in the case of numerical integratio n by discrete steps. Furthermore, a proper evaluation of the diffusion coef ficient is obtained by a numerical simulation of transport in anisotropic m agnetic turbulence. The scaling of the fluctuation level and of the correla tion lengths with the distance from the Sun are also taken into account. As a consequence, plasma transport across the average magnetic field directio n is obtained. An application to the propagation of energetic particles fro m corotating interacting regions to high heliographic latitudes is consider ed.