The effect of magnetic turbulence on the structure of magnetic field lines is important to understand how the energetic particles propagate in the heliosphere. If the characteristics of the solar wind are known, with the help of spacecraft measures like turbulence spectral index, anisotropy and correlation lengths, solar wind speed, and structure of the average magnetic field, it is possible to reconstruct the magnetic connection between the Sun and the Earth. We evaluate the field line trajectories in solar wind, by integrating the magnetic field line with a Monte Carlo simulation. During the calculation, a perturbation simulating diffusive transport is added to the average Parker spiral magnetic field. In this way maps of the potentially dangerous zones of the Sun are provided, determining at which locations particles accelereted by a flare or a coronal mass ejection could reach the Earth. We find that the position and the angular size of the zone connected to the Earth depends in a sensitive way on the heliomagnetic latitude of the Earth.
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