Thus, near the maximum of solar activity, the magnetic field lines in the overshoot region are horizontal but they are tilted to the meridians. At that time the Sun resembles a ball of twine. Thus, although magnetic fields in the overshoot region remain mostly horizontal, they become highly twisted and braided. The magnetic fields also get organized into isolated flux tubes. The mutual action of the differential rotation and twist amplifies the magnetic field.
Magnetic fields remain frozen-in the solar plasma throughout the convective zone.
At the top of each convective cell, plasma flows from the center of the cell toward its boundary. The chromospheric network commonly observed on the quiet Sun is the result of this flux redistribution by the supergranular convective motions. The typical horizontal size of the supergranular cells is about 20,000 km and every cell is surrounded by a vertical magnetic field. If the vertical size of the supergranular cell is close to its horizontal size, one should expect to see mostly vertical magnetic fields, concentrated in the boundaries of the supergranular cells up to about 20,000 km under the photosphere. Below that, the magnetic field is, probably, not so regular.