  We have examined the global structure of the solar magnetic field using data
from the FeI spectral line at {\lambda}5250.2{\AA} obtained at the 150-foot
tower telescope at the Mt. Wilson Observatory (MWO). For each point on the
solar surface, we find the value of the magnetic field in the meridional plane,
Bm, by averaging over all available observations using a cosine weighting
method. We have revised our cosine weighting method by now taking into account
more fully the highest latitude geometry. We use the annual variation in the
latitude of the disk center, b0, to deduce the tilt angle of the field relative
to the local vertical so that we can find the radial component of the field, Br
from Bm. We find this tilt angle to be small except for a near-polar zone where
a tilt-angle model can reduce the annual variation. The reduced annual
variation in the deduced Br allows us to study dBr/dt and associated deviations
in Br from a smoothed Br with a smoothing width of 2.5 years. These functions
make evident the presence of small amplitude (3 to 5 gauss) but spatially
coherent ripples with a semi-regular periodicity of 1 to 3 years. At any given
time the half-wavelength (peak-to-trough) is between 15 and 30 degrees of
latitude. These patterns are ubiquitous and in many cases drift from near the
equator to the poles over a time period of roughly 2 years. The drift rate
pattern is not compatible with simple advection.
