3D MHD simulation of polarized emission in SN 1006

Abstract

We use three dimensional magnetohydrodynamic (MHD) simulations to model the supernova remnant SN 1006. From our numerical results, we have carried out a polarization study, obtaining synthetic maps of the polarized intensity, the Stokes parameter $Q$, and the polar-referenced angle, which can be compared with observational results. Synthetic maps were computed considering two possible particle acceleration mechanisms: quasi-parallel and quasi-perpendicular. The comparison of synthetic maps of the Stokes parameter $Q$ maps with observations proves to be a valuable tool to discern unambiguously which mechanism is taking place in the remnant of SN 1006, giving strong support to the quasi-parallel model.

6 pages, 4 figures, accepted by MNRAS

References in corpus (5)

• Variation of cosmic ray injection across supernova shocks
• On the Origin of Asymmetries in Bilateral Supernova Remnants
• The gas density around SN 1006
• Aspect angle for interstellar magnetic field in SN 1006
• The dynamics of internal working surfaces in MHD jets

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• A 3D MHD simulation of SN 1006: a polarized emission study for the turbulent case
• Simulating TeV gamma-ray morphologies of shell-type supernova remnants
• Radio polarization maps of shell-type SNRs II. Sedov models with evolution of turbulent magnetic field
• Evolving Supernova Remnants in Multiphase Interstellar Media
• Origin of the bilateral structure of the supernova remnant G296.5+10