First direct measurements of transverse waves in solar polar plumes using SDO/AIA

TL;DR

This study provides the first direct measurements of transverse wave motions in solar polar plumes using SDO/AIA, revealing that these waves are insufficient alone to account for solar wind acceleration.

Contribution

It presents the first direct observational measurements of transverse waves in solar polar plumes, quantifying their properties and energy flux, which challenges previous assumptions about their role in solar wind acceleration.

Findings

Measured transverse displacements, periods, and velocities of 596 oscillations.

Wave energy flux is 4-10 times below the energy needed for solar wind acceleration.

Wave parameters follow log-normal distributions with specific peaks.

Abstract

There is intense interest in determining the precise contribution of Alfv\'enic 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 off-limb solar polar plumes and recently McIntosh et al. (2011, Nature, 475, 477) 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 letter reports on the first direct measurements of transverse wave motions in solar polar plumes. Over a 4 hour period, we measure the transverse displacements, periods and velocity amplitudes of 596 distinct oscillations observed in the 171 \AA channel of SDO/AIA. We find a broad range of non-uniformly distributed parameter values which are well described by log-normal distributions with peaks at $234$ km, $121$ s and $8$ km s$^{-1}$, and mean and standard deviations of $407\pm297$ km, $173\pm118$ s and $14\pm10$ km s$^{-1}$. Within standard deviations, our direct measurements are broadly consistent with previous results. However, accounting for the whole of our observed non-uniform parameter distribution we calculate an energy flux of $9-24$ W m$^{-2}$, which is $4-10$ times below the energy requirement for solar wind acceleration. Hence, our results indicate that transverse MHD waves as resolved by SDO/AIA cannot be the dominant energy source for fast solar wind acceleration in the open-field corona.