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.

arXiv comment6 pages, 4 figures, accepted by MNRAS

References in corpus (14)

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• Variation of cosmic ray injection across supernova shocks
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• Gamma-Ray Burst Dynamics and Afterglow Radiation from Adaptive Mesh Refinement, Special Relativistic Hydrodynamic Simulations
• The gas density around SN 1006
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• MHD simulations of radiative jets from young stellar objects: Halpha emission
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Cited by in corpus (19)

• The Connection between Supernova Remnants and the Galactic Magnetic Field: A Global Radio Study of the Axisymmetric Sample
• Radio polarization maps of shell-type SNRs I. Effects of a random magnetic field component, and thin-shell models
• Kinetic simulations of nonrelativistic perpendicular shocks of young supernova remnants. I. Electron shock-surfing acceleration
• When disorder looks like order: a new model to explain radial magnetic fields in young supernova remnants
• Evolution and observational signatures of the cosmic ray electron spectrum in SN 1006
• Kinetic simulations of nonrelativistic perpendicular shocks of young supernova remnants. II. Influence of shock-surfing acceleration on downstream electron spectra
• Non-thermal radio supernova remnants of exiled Wolf-Rayet stars
• The connection between supernova remnants and the Galactic magnetic field: An analysis of quasi-parallel and quasi-perpendicular cosmic ray acceleration for the axisymmetric sample
• A 3D MHD simulation of SN 1006: a polarized emission study for the turbulent case
• A Study of Radio Polarization in Protostellar Jets
• 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
• New perspectives on the supernova remnant Puppis A based on a radio polarization study
• Supernova of 1006 (G327.6+14.6)
• Evolving Supernova Remnants in Multiphase Interstellar Media
• Origin of the bilateral structure of the supernova remnant G296.5+10
• On the Potential of Faraday Tomography to Identify Shock Structures in Supernova Remnants
• 3D MHD simulations of the supernova remnant CTB 109
• The mechanism of efficient electron acceleration at parallel non-relativistic shocks