  The propagating intensity disturbances (PIDs) in plumes are still poorly
understood and their identity (magnetoacoustic waves or flows) remains an open
question. We investigate PIDs in five plumes located in the northern polar
coronal hole observed during the 2017 total solar eclipse. Three plumes are
associated with coronal bright points, jets and macrospicules at their base
(active plumes) and the other two plumes are not (quiet plumes). The electron
temperature at the base of the plumes is obtained from the filter ratio of
images taken with the X-ray Telescope on board Hinode and the passband ratio
around 400 nm from an eclipse instrument, the Diagnostic Coronagraph Experiment
(DICE). The phase speed (v_r), frequency (omega), and wavenumber (k) of the
PIDs in the plumes are obtained by applying a Fourier transformation to the
space-time (r-t plane) plots in images taken with the Atmospheric Imaging
Assembly (AIA) in three different wavelength channels (171 A, 193 A, and 211
A). We found that the PIDs in the higher temperature AIA channels, 193 and 211
A, are faster than that of the cooler AIA 171 A channel. This tendency is more
significant for the active plumes than the quiet ones. The observed speed ratio
(~1.3) between the AIA 171 and 193 A channels is similar to the theoretical
value (1.25) of a slow magnetoacoustic wave. Our results support the idea that
PIDs in plumes represent a superposition of slow magnetoacoustic waves and
plasma outflows that consist of dense cool flows and hot coronal jets.
