  We show that simulations of magnetohydrodynamic turbulence in the multiphase
interstellar medium yield an $E/B$ ratio for polarized emission from Galactic
dust in broad agreement with recent $Planck$ measurements. In addition, the
$B$-mode spectra display a scale dependence that is consistent with
observations over the range of scales resolved in the simulations. The
simulations present an opportunity to understand the physical origin of the
$E/B$ ratio, and a starting point for more refined models of Galactic emission
of use for both current and future CMB experiments.
