Origin of the bilateral structure of the supernova remnant G296.5+10

Autores
Moranchel-Basurto, A.; Velazquez, P.; Giacani, Elsa Beatriz; Toledo Roy, J. C.; Schneiter, E.; De Colle, F.; Esquivel, A.
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
In this work, we have modelled the supernova remnant (SNR) G296.5+10, by means of 3D magnetohydrodynamics (MHD) simulations. This remnant belongs to the bilateral SNR group and has an additional striking feature: the rotation measure (RM) in its eastern and western parts are very different. In order to explain both the morphology observed in radio-continuum and the RM, we consider that the remnant expands into a medium shaped by the superposition of the magnetic field of the progenitor star with a constant Galactic magnetic field. We have also carried out a polarization study from our MHD results, obtaining synthetic maps of the linearly polarized intensity and the Stokes parameters. This study reveals that both the radio morphology and the reported RM for G296.5+10 can be explained if the quasi-parallel acceleration mechanism is taking place in the shock front of this remnant.
Fil: Moranchel-Basurto, A.. Universidad Nacional Autónoma de México; México
Fil: Velazquez, P.. Universidad Nacional Autónoma de México; México
Fil: Giacani, Elsa Beatriz. Universidad de Buenos Aires. Facultad de Arquitectura y Urbanismo; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Toledo Roy, J. C.. Universidad Nacional Autónoma de México; México
Fil: Schneiter, E.. Universidad Nacional Autónoma de México; México
Fil: De Colle, F.. Universidad Nacional Autónoma de México; México
Fil: Esquivel, A.. Universidad Nacional Autónoma de México; México
Materia
RADIATION MECHANISMS:NON-THERMAL
SUPERNOVA REMNANTS
MHD, METHODS:NUMERICAL
SHOCK WAVES
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/29693
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/29693
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Origin of the bilateral structure of the supernova remnant G296.5+10Moranchel-Basurto, A.Velazquez, P.Giacani, Elsa BeatrizToledo Roy, J. C.Schneiter, E.De Colle, F.Esquivel, A.RADIATION MECHANISMS:NON-THERMALSUPERNOVA REMNANTSMHD, METHODS:NUMERICALSHOCK WAVEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1In this work, we have modelled the supernova remnant (SNR) G296.5+10, by means of 3D magnetohydrodynamics (MHD) simulations. This remnant belongs to the bilateral SNR group and has an additional striking feature: the rotation measure (RM) in its eastern and western parts are very different. In order to explain both the morphology observed in radio-continuum and the RM, we consider that the remnant expands into a medium shaped by the superposition of the magnetic field of the progenitor star with a constant Galactic magnetic field. We have also carried out a polarization study from our MHD results, obtaining synthetic maps of the linearly polarized intensity and the Stokes parameters. This study reveals that both the radio morphology and the reported RM for G296.5+10 can be explained if the quasi-parallel acceleration mechanism is taking place in the shock front of this remnant.Fil: Moranchel-Basurto, A.. Universidad Nacional Autónoma de México; MéxicoFil: Velazquez, P.. Universidad Nacional Autónoma de México; MéxicoFil: Giacani, Elsa Beatriz. Universidad de Buenos Aires. Facultad de Arquitectura y Urbanismo; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Toledo Roy, J. C.. Universidad Nacional Autónoma de México; MéxicoFil: Schneiter, E.. Universidad Nacional Autónoma de México; MéxicoFil: De Colle, F.. Universidad Nacional Autónoma de México; MéxicoFil: Esquivel, A.. Universidad Nacional Autónoma de México; MéxicoOxford University Press2017-08-14info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/29693Moranchel-Basurto, A.; Velazquez, P.; Giacani, Elsa Beatriz; Toledo Roy, J. C.; Schneiter, E.; et al.; Origin of the bilateral structure of the supernova remnant G296.5+10; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 472; 2; 14-8-2017; 2117-21250035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/472/2/2117/4082238?redirectedFrom=fulltextinfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx2086info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:52:01Zoai:ri.conicet.gov.ar:11336/29693instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:52:01.348CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Origin of the bilateral structure of the supernova remnant G296.5+10
title Origin of the bilateral structure of the supernova remnant G296.5+10
spellingShingle Origin of the bilateral structure of the supernova remnant G296.5+10
Moranchel-Basurto, A.
RADIATION MECHANISMS:NON-THERMAL
SUPERNOVA REMNANTS
MHD, METHODS:NUMERICAL
SHOCK WAVES
title_short Origin of the bilateral structure of the supernova remnant G296.5+10
title_full Origin of the bilateral structure of the supernova remnant G296.5+10
title_fullStr Origin of the bilateral structure of the supernova remnant G296.5+10
title_full_unstemmed Origin of the bilateral structure of the supernova remnant G296.5+10
title_sort Origin of the bilateral structure of the supernova remnant G296.5+10
dc.creator.none.fl_str_mv Moranchel-Basurto, A.
Velazquez, P.
Giacani, Elsa Beatriz
Toledo Roy, J. C.
Schneiter, E.
De Colle, F.
Esquivel, A.
author Moranchel-Basurto, A.
author_facet Moranchel-Basurto, A.
Velazquez, P.
Giacani, Elsa Beatriz
Toledo Roy, J. C.
Schneiter, E.
De Colle, F.
Esquivel, A.
author_role author
author2 Velazquez, P.
Giacani, Elsa Beatriz
Toledo Roy, J. C.
Schneiter, E.
De Colle, F.
Esquivel, A.
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv RADIATION MECHANISMS:NON-THERMAL
SUPERNOVA REMNANTS
MHD, METHODS:NUMERICAL
SHOCK WAVES
topic RADIATION MECHANISMS:NON-THERMAL
SUPERNOVA REMNANTS
MHD, METHODS:NUMERICAL
SHOCK WAVES
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv In this work, we have modelled the supernova remnant (SNR) G296.5+10, by means of 3D magnetohydrodynamics (MHD) simulations. This remnant belongs to the bilateral SNR group and has an additional striking feature: the rotation measure (RM) in its eastern and western parts are very different. In order to explain both the morphology observed in radio-continuum and the RM, we consider that the remnant expands into a medium shaped by the superposition of the magnetic field of the progenitor star with a constant Galactic magnetic field. We have also carried out a polarization study from our MHD results, obtaining synthetic maps of the linearly polarized intensity and the Stokes parameters. This study reveals that both the radio morphology and the reported RM for G296.5+10 can be explained if the quasi-parallel acceleration mechanism is taking place in the shock front of this remnant.
Fil: Moranchel-Basurto, A.. Universidad Nacional Autónoma de México; México
Fil: Velazquez, P.. Universidad Nacional Autónoma de México; México
Fil: Giacani, Elsa Beatriz. Universidad de Buenos Aires. Facultad de Arquitectura y Urbanismo; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Toledo Roy, J. C.. Universidad Nacional Autónoma de México; México
Fil: Schneiter, E.. Universidad Nacional Autónoma de México; México
Fil: De Colle, F.. Universidad Nacional Autónoma de México; México
Fil: Esquivel, A.. Universidad Nacional Autónoma de México; México
description In this work, we have modelled the supernova remnant (SNR) G296.5+10, by means of 3D magnetohydrodynamics (MHD) simulations. This remnant belongs to the bilateral SNR group and has an additional striking feature: the rotation measure (RM) in its eastern and western parts are very different. In order to explain both the morphology observed in radio-continuum and the RM, we consider that the remnant expands into a medium shaped by the superposition of the magnetic field of the progenitor star with a constant Galactic magnetic field. We have also carried out a polarization study from our MHD results, obtaining synthetic maps of the linearly polarized intensity and the Stokes parameters. This study reveals that both the radio morphology and the reported RM for G296.5+10 can be explained if the quasi-parallel acceleration mechanism is taking place in the shock front of this remnant.
publishDate 2017
dc.date.none.fl_str_mv 2017-08-14
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/29693
Moranchel-Basurto, A.; Velazquez, P.; Giacani, Elsa Beatriz; Toledo Roy, J. C.; Schneiter, E.; et al.; Origin of the bilateral structure of the supernova remnant G296.5+10; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 472; 2; 14-8-2017; 2117-2125
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/29693
identifier_str_mv Moranchel-Basurto, A.; Velazquez, P.; Giacani, Elsa Beatriz; Toledo Roy, J. C.; Schneiter, E.; et al.; Origin of the bilateral structure of the supernova remnant G296.5+10; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 472; 2; 14-8-2017; 2117-2125
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/472/2/2117/4082238?redirectedFrom=fulltext
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx2086
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 12.982451

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