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Nonlinear Processes in Geophysics An interactive open-access journal of the European Geosciences Union
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Volume 8, issue 3
Nonlin. Processes Geophys., 8, 151–158, 2001
https://doi.org/10.5194/npg-8-151-2001
© Author(s) 2001. This work is licensed under
the Creative Commons Attribution-NonCommercial-ShareAlike 2.5 License.

Special issue: Theory and simulation of Solar System Plasmas, No. 2

Nonlin. Processes Geophys., 8, 151–158, 2001
https://doi.org/10.5194/npg-8-151-2001
© Author(s) 2001. This work is licensed under
the Creative Commons Attribution-NonCommercial-ShareAlike 2.5 License.

  30 Jun 2001

30 Jun 2001

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

P. Pommois, G. Zimbardo, and P. Veltri P. Pommois et al.
  • Dipartimento di Fisica, Università della Calabria, and Istituto Nazionale per la Fisica della Materia, Unità di Cosenza, I-87030 Arcavacata di Rende, Italy

Abstract. It is well known that the structure of magnetic field lines in solar wind can be influenced by the presence of the magnetohydrodynamic turbulence. We have developed a Monte Carlo simulation which traces the magnetic field lines in the heliosphere, including the effects of magnetic turbulence. These effects are modelled by random operators which are proportional to the square root of the magnetic field line diffusion coefficient. The modelling of the random terms is explained, in detail, in the case of numerical integration by discrete steps. Furthermore, a proper evaluation of the diffusion coefficient is obtained by a numerical simulation of transport in anisotropic magnetic turbulence. The scaling of the fluctuation level and of the correlation lengths with the distance from the Sun are also taken into account. As a consequence, plasma transport across the average magnetic field direction is obtained. An application to the propagation of energetic particles from corotating interacting regions to high heliographic latitudes is considered.

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