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

## TL;DR

This paper presents a detailed model for polarized radio emission from shell-type supernova remnants during their Sedov phase, incorporating turbulent magnetic fields, particle acceleration, and Faraday rotation to produce realistic polarization maps.

## Contribution

It introduces a comprehensive 3D modeling approach for SNR polarization maps, including magnetic turbulence, particle acceleration, and Faraday effects, advancing the simulation of observational data.

## Key findings

- Generated detailed polarization maps for SNRs during Sedov evolution.
- Analyzed effects of magnetic turbulence and Faraday rotation on polarization.
- Provided insights into the magnetic field structure within SNRs.

## Abstract

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