  We examine the dynamical behavior of white light polar plume structures in
the inner corona that are observed from the ground during total solar eclipses,
based on their EUV hot and cool emission line counterparts observed from space.
EUV observations from SDO/AIA of a sequence of rapidly varying coronal hole
structures are analyzed. Evidence of events showing acceleration in the 1.25 Mk
line of Fe XII at 193 A is given. The structures along the plume show an
outward velocity of about 140 kms-1 that can be interpreted as an upwards
propagating wave in the 304 A and 171 A lines; higher speeds are seen in 193 A
(up to 1000 km/s). The ejection of the cold He II plasma is delayed by about 4
min in the lowest layer and more than 12 min in the highest level compared to
the hot 193 A behavior. A study of the dynamics using time-slice diagrams
reveals that a large amount of fast ejected material originates from below the
plume, at the footpoints. The release of plasma material appears to come from a
cylinder with quasi-parallel edge-enhanced walls. After the initial phase of a
longitudinal acceleration, the speed substantially reduces and the ejecta
disperse into the environment. Finally, the detailed temporal and spatial
relationships between the cool and hot components were studied with
simultaneous multi-wavelength observations, using more AIA data. The
outward-propagating perturbation of the presumably magnetic walls of polar
plumes supports the suggestion that Alfven waves propagate outwardly along
these radially extended walls.
