In our previous work, we have studied the horizontal dispersal of magnetic field concentrations on MDI magnetograms. These concentrations are found to be transported over the solar surface, in response to the granular and supergranular motions. Below the surface, the field lines may get braided and intermingled by the flows, which would lead not only to interactions below the surface, but possibly also affect the higher layers. Taking in mind the complicated, extremely dynamic nature of the solar photosphere, describing the 3-dimensional behavior of the magnetic field is not a straightforward task.