# A 3D MHD simulation of SN 1006: a polarized emission study for the turbulent case

## TL;DR

This paper uses 3D MHD simulations to analyze the polarized radio emission of SN 1006, demonstrating that turbulence in the interstellar medium can explain observed polarization features and help determine magnetic field orientation.

## Contribution

It introduces a new polarization analysis method based on 3D MHD simulations considering turbulence, improving understanding of magnetic field structures in supernova remnants.

## Key findings

- Turbulent medium with adiabatic index 1.3 reproduces SN 1006 polarization.
- Statistical analysis of magnetic field angles aids in determining ambient magnetic field orientation.
- Simulation results align with observed polarization properties of SN 1006.

## Abstract

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.