Abstract :
Regarding the footpoint motion of magnetic field lines in the solar corona, it is clear that a magnetic pattern in the heliosphere predicted by Fisk is much more complicated than the standard Parker interplanetary magnetic field. At first, in the presented paper the tensor for anisotropic diffusion is converted from the coordinate system dependent on magnetic field lines to the spherical system for a case where the interplanetary magnetic field has 3 components: Br, Bθ, Bϕ. In the next part of the paper the simplified version of Fiskʹs model proposed by Zurbuchen et al. is considered in order to obtain a magnetic field line configuration. The expansion of the Fisk interplanetary field lines in the heliosphere is shown in the case when the lines of force of magnetic field originate from the inclined polar coronal hole and when they originate from an equatorial region. Accepted assumptions concerning the dependence of the diffusion coefficients on the coordinates are discussed.
