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Polarized radio emission has been mapped with great detail in severalGalactic supernova remnants (SNRs), but has not yet been exploited to theextent it deserves. We have developed a method to model maps of the Stokesparameters for shell-like SNRs during their Sedov evolution phase. At first,3-dimensional structure of a SNR has been computed, by modeling thedistribution of the magnetohydrodynamic parameters and of the acceleratedparticles. The generation and dissipation of the turbulent component ofmagnetic field everywhere in SNR are also considered taking into account itsinteraction with accelerated particles. Then, in order to model the emission,we have used a generalization of the classical synchrotron theory, valid forthe case in which the magnetic field has ordered and disordered components.Finally, 2-dimensional projected maps have been derived, for differentorientations of SNR and of interstellar magnetic field with respect to theobserver. An important effect to consider is the Faraday rotation of thepolarization planes inside the SNR interior. In this paper we present detailsof the model, and describe general properties of the images.

Radio polarization maps of shell-type SNRs II. Sedov models with evolution of turbulent magnetic field