An MHD study of SN 1006 and determination of the ambient magnetic field direction

In this work, we employ a magnetohydrodynamic (MHD) numerical code to reproduce the morphology observed for SN 1006 in radio synchrotron and thermal X-ray emission. We introduce a density discontinuity, in the form of a flat cloud parallel to the Galactic plane, in order to explain the NW filament o...

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Detalles Bibliográficos
Publicado: 2010
Materias:
ISM: supernova remnants
Methods: numerical
MHD
Radiation mechanisms: general
Supernovae: individual: SN 1006
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v408_n1_p430_Schneiter
http://hdl.handle.net/20.500.12110/paper_00358711_v408_n1_p430_Schneiter
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00358711_v408_n1_p430_Schneiter
record_format dspace
spelling paper:paper_00358711_v408_n1_p430_Schneiter2023-06-08T15:01:29Z An MHD study of SN 1006 and determination of the ambient magnetic field direction ISM: supernova remnants Methods: numerical MHD Radiation mechanisms: general Supernovae: individual: SN 1006 In this work, we employ a magnetohydrodynamic (MHD) numerical code to reproduce the morphology observed for SN 1006 in radio synchrotron and thermal X-ray emission. We introduce a density discontinuity, in the form of a flat cloud parallel to the Galactic plane, in order to explain the NW filament observed in optical wavelengths and in thermal X-rays. We compare our models with observations. We also perform a test that contrasts the radio emitting bright limbs of the supernova remnant against the central region, finding additional support to our results. Our main conclusion is that the most probable direction of the ambient magnetic field is on average perpendicular to the Galactic plane. © 2010 The Authors. Journal compilation © 2010 RAS. 2010 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v408_n1_p430_Schneiter http://hdl.handle.net/20.500.12110/paper_00358711_v408_n1_p430_Schneiter
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic ISM: supernova remnants
Methods: numerical
MHD
Radiation mechanisms: general
Supernovae: individual: SN 1006
spellingShingle ISM: supernova remnants
Methods: numerical
MHD
Radiation mechanisms: general
Supernovae: individual: SN 1006
An MHD study of SN 1006 and determination of the ambient magnetic field direction
topic_facet ISM: supernova remnants
Methods: numerical
MHD
Radiation mechanisms: general
Supernovae: individual: SN 1006
description In this work, we employ a magnetohydrodynamic (MHD) numerical code to reproduce the morphology observed for SN 1006 in radio synchrotron and thermal X-ray emission. We introduce a density discontinuity, in the form of a flat cloud parallel to the Galactic plane, in order to explain the NW filament observed in optical wavelengths and in thermal X-rays. We compare our models with observations. We also perform a test that contrasts the radio emitting bright limbs of the supernova remnant against the central region, finding additional support to our results. Our main conclusion is that the most probable direction of the ambient magnetic field is on average perpendicular to the Galactic plane. © 2010 The Authors. Journal compilation © 2010 RAS.
title An MHD study of SN 1006 and determination of the ambient magnetic field direction
title_short An MHD study of SN 1006 and determination of the ambient magnetic field direction
title_full An MHD study of SN 1006 and determination of the ambient magnetic field direction
title_fullStr An MHD study of SN 1006 and determination of the ambient magnetic field direction
title_full_unstemmed An MHD study of SN 1006 and determination of the ambient magnetic field direction
title_sort mhd study of sn 1006 and determination of the ambient magnetic field direction
publishDate 2010
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v408_n1_p430_Schneiter
http://hdl.handle.net/20.500.12110/paper_00358711_v408_n1_p430_Schneiter
_version_ 1768546338009513984

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