Density Fluctuations in a Polar Coronal Hole

We have measured the root-mean-square (rms) amplitude of intensity fluctuations, Delta I, in plume and interplume regions of a polar coronal hole. These intensity fluctuations correspond to density fluctuations. Using data from the Sun Watcher using the Active Pixel System detector and Image Processing on the Project for Onboard Autonomy (Proba2), our results extend up to a height of about 1.35. R-circle dot. One advantage of the rms analysis is that it does not rely on a detailed evaluation of the power spectrum, which is limited by noise levels to low heights in the corona. The rms approach can be performed up to larger heights where the noise level is greater, provided that the noise itself can be quantified. At low heights, both the absolute Delta I, and the amplitude relative to the mean intensity, Delta I/I, decrease with height. However, starting at about 1.2. Re-circle dot, Delta I/I increases, reaching 20%-40% by 1.35. R-circle dot. This corresponds to density fluctuations of Delta n(e)/n(e) approximate to 10%-20%. The increasing relative amplitude implies that the density fluctuations are generated in the corona itself. One possibility is that the density fluctuations are generated by an instability of Alfven waves. This generation mechanism is consistent with some theoretical models and with observations of Alfven wave amplitudes in coronal holes. Although we find that the energy of the observed density fluctuations is small, these fluctuations are likely to play an important indirect role in coronal heating by promoting the reflection of Alfven waves and driving turbulence.