  Three dimensional magnetohydrodynamical simulations were carried out in order
to perform a new polarization study of the radio emission of the supernova
remnant SN 1006. These simulations consider that the remnant expands into a
turbulent interstellar medium (including both magnetic field and density
perturbations). Based on the referenced-polar angle technique, a statistical
study was done on observational and numerical magnetic field position-angle
distributions. Our results show that a turbulent medium with an adiabatic index
of 1.3 can reproduce the polarization properties of the SN 1006 remnant. This
statistical study reveals itself as a useful tool for obtaining the orientation
of the ambient magnetic field, previous to be swept up by the main supernova
remnant shock.
