There is intense interest in determining the precise contribution of Alfvénic waves propagating along solar structures to the problems of coronal heating and solar wind acceleration. Since the launch of SDO/AIA, it has been possible to resolve transverse oscillations in offlimb solar polar plumes and recently McIntosh et al. concluded that such waves are energetic enough to play a role in heating the corona and accelerating the fast solar wind. However, this result is based on comparisons to Monte Carlo simulations and confirmation via direct measurements is still outstanding. Thus, this presentation reports on the first direct measurements of transverse wave motions in solar polar plumes. Over a four hour period, we measure the transverse displacements, periods, and velocity amplitudes of 596 distinct oscillations observed in the 171 Å channel of SDO/AIA. We find a broad range of nonuniformly distributed parameter values which are well described by lognormal distributions with peaks at 234 km, 121 s, and 8 km/s, and mean and standard deviations of 407 ± 297 km, 173 ± 118 s, and 14 ± 10 km/s. Within standard deviations, our direct measurements are broadly consistent with previous results. However, accounting for the whole of our observed nonuniform parameter distribution we calculate an energy flux of 924 W/m^2, which is 410 times below the energy requirement for solar wind acceleration. Hence, our results indicate that transverse magnetohydrodynamic waves as resolved by SDO/AIA cannot be the dominant energy source for fast solar wind acceleration in the openfield corona.
