The random walk of Interplanetary Magnetic Field lines due to the intersupergranular magnetic flux tubes and its effect on the transport of the Solar Energetic Particles in the inner Heliosphere

Parker, 1968, introduced the spiral magnetic field model by assumption of radially outward solar wind, solar rotation and fixed footpoint scheme in the photosphere. Even though the observations (Forsyth et al., 1996) confirmed that the average magnetic field is parker, the photosphere shows variety of advecting flows which have also a variety of spatial scales from small, Granular, flows to large scales such as, Supergranular, Giant cells, differential rotation and Meriodinal flows that led us to believe that the field lines are nonparker. These advecting flows can cause the random walk of footpoints that leads to the meandering of the field lines. However, the open field magnetic flux tubes are only emerging from the intersupergranular space between three or more supergranules and rise up to the source surface in the lower corona. This study, tries to introduce a model for simulating the source surface velocity spectrum from the photosphere's velocity spectrum and its effect on the Interplanetary Magnetic Field, IPM, and the transport of Solar Energetic Particles in the energy range of a few tens of MeV to a few hundreds of MeV.