Thomson et al. suggest that the wind flowing from the Sun contains many discrete, identifiable modes corresponding to solar internal pressure (p) and gravity (g) modes, in sharp contrast to the standard paradigm of the solar wind as a turbulently evolving magnetofluid with a continuous spectrum of modes. Here we argue for the continuum assumption, and show that the spatio-temporal variation of the solar surface and atmosphere will not allow well-defined modes to persist in the wind, except at low frequencies, where solar-rotation periods and their harmonics account for at least most of the spectral peaks.
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