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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/29693
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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 Técnicas2025-09-29T10:19:18Zoai: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:34982025-09-29 10:19:19.146CONICET 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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1844614163868942336 |
score |
13.070432 |