Due to turbulence in the
presence of rotation in stellar
convection zones, the buoyantly rising flux tubes are twisted into the
meridional plane, producing the poloidal field.
Due to the Coriolis force, the
rising flux tubes will
be twisted slightly, making bipolar sunspot pairs appear tilted. On the
surface the sunspot pairs will decay spreading the magnetic field,
which
will cancel out with its opposite helisphere counterparts in the lower
lattitudes, but become stronger in the higher latitudes reversing the
old
polarity and creating new poloidal field.
