Dust-polarization maps for local interstellar turbulence

We show that simulations of magnetohydrodynamic turbulence in the multiphase interstellar medium yield an $E\mathrm{/}B$ 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 $E\mathrm{/}B$ ratio, and a starting point for more refined models of Galactic emission of use for both current and future CMB experiments.