  This paper uses wavelet transforms to look for the rotational frequencies of
the Sun's mean line-of-sight magnetic field. For a sufficiently high wavelet
frequency, the spectra of the dipole, quadrupole, and hexapole field components
each show a time-dependent fine structure with periods in the range of 26.5-30
days and their harmonics. These maps confirm that a large enhancement of 30-day
power occurred in the dipole field during 1989-1990, as recorded previously
using Fourier techniques (Sheeley 2022). Also, during some years the maps show
power at 26.5 days (or its harmonics), that is clearly distinguishable from the
26.9-27.0 day rotation period at the Sun's equator. In at least one case, the
26.5-day period was a wave phenomenon caused by the systematic eruption of
active regions at progressively more western locations in the Carrington
coordinate system, as if the flux were emerging from a fixed longitude in a
faster rotating subsurface layer. Based on previous studies of the mean field
(Sheeley et al 1985, Sheeley & DeVore 1986, Sheeley 2022), I conclude that the
enhanced wavelet patterns in this paper are regions where magnetic flux is
emerging in configurations that strengthen the Sun's horizontal dipole,
quadrupole, and hexapole fields, and (in the case of the more slowly rotating
patterns) where this flux is being transported to mid-latitudes whose rotation
periods are in the range 28-30 days.
