  Rotation of the large scale solar magnetic field has a great importance for
the understanding of solar dynamic, for the search of longitidinal structure
and for the study of solar-terrestrial relations. 30-year long observations
taken at the Wilcox Solar Observatory (USA) in 21-23 cycles have been analysed
carefully to deduce magnetic field rotation rate at different latitudes in both
hemispheres and its variability in time. The WSO data appear to indicate that
additionally to the differential rotation along the latitudes there are running
waves of fast rotation of the magnetic field. These torsional waves are running
from the poles to the equator with a period of 11 years. The rotation of the
magnetic field (RMF) is almost rigid at latitudes above 55 degrees in both
hemispheres. The rotation rate in the sub-polar regions is slower when the
magnetic field is strong there (during minima of solar activity), and faster
when the magnetic field changes polarity (during maxima of solar activity).
