  Recent Planck observations of dust polarization in the Galaxy have revealed
that the power in $E$ mode is twice that in $B$ mode. Caldwell et. al. have
formulated a theoretical model in the context of magnetohydrodynamic (MHD)
turbulence and found it problematic to account for this result. In particular,
they concluded that there is a very narrow range of theoretical parameters that
could account for the observation. This poses a problem of whether the accepted
description of MHD turbulence can apply to the interstellar medium. We revisit
the problem and demonstrate that MHD turbulence corresponding to the high
galactic latitudes range of Alfv\'en Mach numbers, i.e. $M_A\lesssim 0.5$, can
successfully explain the available results for the $E$ to $B$ mode ratio.
