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

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.

8 pages, 7 figures, accepted for publication in MNRAS

References in corpus (2)

• 3D MHD simulation of polarized emission in SN 1006
• The dynamics of internal working surfaces in MHD jets

Cited by in corpus (4)

• When disorder looks like order: a new model to explain radial magnetic fields in young supernova remnants
• Non-thermal radio supernova remnants of exiled Wolf-Rayet stars
• Origin of the bilateral structure of the supernova remnant G296.5+10
• Numerically investigating the morphology of the supernova remnant SN 1006 in the ambient medium with a density discontinuity