I created a model of polarized emission from dust grains aligned with the galactic
magnetic field for comparison with Planck observations. I modeled the magnetic field in
the galactic disk as a field with a cylindrical constant component and an equal strength
random component. I investigated how the fractional polarization down a line of sight
varies with different models of a random field. I determine that different models of
random fields yield different amounts of fractional polarization, especially over sightlines
longer than a decorrelation length.