  Coronal hole spatial-temporal evolution is studied and comparison made with
that of the solar global magnetic field in cycles 21-23 (1976-2012). The
latitude-longitude distribution dynamics of coronal holes and the regularities
in the global magnetic field associated with the solar polar field reversal are
analyzed. Polar and non-polar coronal hole populations are considered. The
investigation reveals some temporal and spatial regularities in coronal hole
distributions that match well the global magnetic-field cycle evolution. The
results show that the non-polar coronal hole longitudinal distribution follows
all configuration changes in the global magnetic-field structure.
Reorganizations of the global magnetic-field and coronal hole distributions
occur simultaneously during a time interval of a few solar rotations. The cycle
evolution of the non-polar coronal holes reflects the transition of the solar
global magnetic field from the zonal structure to sectorial andvice versa. Two
different type waves of non-polar coronal holes are revealed from their
latitudinal distribution. The first one is short poleward waves. They trace the
poleward motion of the unipolar photospheric magnetic fields from approximately
35 deg to the associated pole in each hemisphere and the redevelopment of a
new-polarity polar CH. Although they start the poleward movement before the
change of the polar magnetic field in the associated hemisphere, they reach the
pole after the polar reversal. The other type of non-polar CH wave forms two
sinusoidal branches associated with the positive- and negative-polarity
magnetic fields. The complete period of the wave was equal to approximately 268
CRs (22 years). These wave CHs arrive at high latitudes during declining phases
when the new polarity polar CHs are already completely formed.
