We study the meridional flow of small magnetic features, using high-re
solution magnetograms taken from 1978 to 1990 with the NSO Vacuum Tele
scope on Kitt Peak. Latitudinal motions are determined by a two-dimens
ional crosscorrelation analysis of 514 pairs of consecutive daily obse
rvations from which active regions are excluded. We find a meridional
flow of the order of 10 m s-1, which is poleward in each hemisphere, i
ncreases in amplitude from 0 at the equator, reaches a maximum at mid-
latitude, and slowly decreases poleward. The average observed meridion
al flow is fit adequately by an expansion of the form M(theta) = 12.9(
+/-0.6) sin(2theta) + 1.4(+/-0.6) sin(4theta), in m s-1 where theta is
the latitude and which reaches a maximum of 13.2 m s-1 at 39-degrees.
We also find a solar-cycle dependence of the meridional flow. The flo
w remains poleward during the cycle, but the amplitude changes from sm
aller-than-average during cycle maximum to larger-than-average during
cycle minimum for latitudes between about 15-degrees and 45-degrees. T
he difference in amplitude between the flows at cycle minimum and maxi
mum depends on latitude and is about 25% of the grand average value. T
he change of the flow amplitude from cycle maximum to minimum occurs r
apidly, in about one year, for the 15-45-degrees latitude range. At th
e highest latitude range analyzed, centered at 52.5-degrees, the flow
is more poleward-than-average during minimum and maximum, and less at
other times. These data show no equatorward migration of the meridiona
l flow pattern during the solar cycle and no significant hemispheric a
symmetry. Our results agree with the meridional flow and its temporal
variation derived from Doppler data. They also agree on average with t
he meridional flow derived from the poleward migration of the weak lar
ge-scale magnetic field patterns but differ in the solar-cycle depende
nce. Our results, however, disagree with the meridional flow derived f
rom sunspots or plages.