3D MHD simulation of polarized emission in SN 1006
We use three-dimensional magnetohydrodynamic 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 wi...
| Authors: | ; ; ; ; |
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| Format: | Article |
| Status: | Published version |
| Publication date: | 2015 |
| Country: | Argentina |
| Institution: | Consejo Nacional de Investigaciones Científicas y Técnicas |
| Repository: | CONICET Digital (CONICET) |
| Language: | English |
| OAI Identifier: | oai:ri.conicet.gov.ar:11336/17373 |
| Online Access: | http://hdl.handle.net/11336/17373 |
| Access Level: | Open access |
| Keyword: | MHD radiation mechanisms: general methods: numerical supernovae: individual: SN 1006 ISM: supernova remnants https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| Summary: | We use three-dimensional magnetohydrodynamic 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. |
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