Rectangular core-collapse supernova remnants: Application to Puppis A

Autores
Meyer, D. M. A.; Velázquez, Pablo F.; Petruk, Oleg; Chiotellis, Alexandros; Pohl, Michael; Camps Fariña, A.; Petrov, M.; Reynoso, Estela Marta; Toledo Roy, J. C.; Schneiter, Ernesto Matías; Castellanos Ramírez, A.; Esquivel, Alejandro
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n ≈ 1 cm-3, T ≈ 8000 K), an organized magnetic field of strength 7μ G has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper, we show through 2.5D magnetohydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 M⊙ that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15-20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetized, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse-Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A.
Fil: Meyer, D. M. A.. Universitat Potsdam; Alemania
Fil: Velázquez, Pablo F.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Petruk, Oleg. No especifíca;
Fil: Chiotellis, Alexandros. National Observatory Of Athens; Grecia
Fil: Pohl, Michael. Universitat Potsdam; Alemania
Fil: Camps Fariña, A.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México. Universidad Complutense de Madrid; España
Fil: Petrov, M.. Max Planck Computing And Data Facility; Alemania
Fil: Reynoso, Estela Marta. Consejo Nacional de Investigaciones 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. Instituto de Ciencias Nucleares; México
Fil: Schneiter, Ernesto Matías. Universidad Nacional de Córdoba. Facultad de Cs.exactas Físicas y Naturales. Departamento de Materiales y Tecnología; Argentina
Fil: Castellanos Ramírez, A.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Esquivel, Alejandro. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Materia
ISM: SUPERNOVA REMNANTS
METHODS: MHD
STARS: EVOLUTION
STARS: MASSIVE
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:11336/216753
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/216753
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Rectangular core-collapse supernova remnants: Application to Puppis AMeyer, D. M. A.Velázquez, Pablo F.Petruk, OlegChiotellis, AlexandrosPohl, MichaelCamps Fariña, A.Petrov, M.Reynoso, Estela MartaToledo Roy, J. C.Schneiter, Ernesto MatíasCastellanos Ramírez, A.Esquivel, AlejandroISM: SUPERNOVA REMNANTSMETHODS: MHDSTARS: EVOLUTIONSTARS: MASSIVEhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n ≈ 1 cm-3, T ≈ 8000 K), an organized magnetic field of strength 7μ G has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper, we show through 2.5D magnetohydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 M⊙ that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15-20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetized, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse-Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A.Fil: Meyer, D. M. A.. Universitat Potsdam; AlemaniaFil: Velázquez, Pablo F.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; MéxicoFil: Petruk, Oleg. No especifíca;Fil: Chiotellis, Alexandros. National Observatory Of Athens; GreciaFil: Pohl, Michael. Universitat Potsdam; AlemaniaFil: Camps Fariña, A.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México. Universidad Complutense de Madrid; EspañaFil: Petrov, M.. Max Planck Computing And Data Facility; AlemaniaFil: Reynoso, Estela Marta. Consejo Nacional de Investigaciones 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. Instituto de Ciencias Nucleares; MéxicoFil: Schneiter, Ernesto Matías. Universidad Nacional de Córdoba. Facultad de Cs.exactas Físicas y Naturales. Departamento de Materiales y Tecnología; ArgentinaFil: Castellanos Ramírez, A.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; MéxicoFil: Esquivel, Alejandro. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; MéxicoWiley Blackwell Publishing, Inc2022-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/216753Meyer, D. M. A.; Velázquez, Pablo F.; Petruk, Oleg; Chiotellis, Alexandros; Pohl, Michael; et al.; Rectangular core-collapse supernova remnants: Application to Puppis A; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 515; 1; 9-2022; 594-6050035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/515/1/594/6628661?redirectedFrom=fulltextinfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac1832info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-12-23T14:04:25Zoai:ri.conicet.gov.ar:11336/216753instacron: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:34982025-12-23 14:04:25.551CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Rectangular core-collapse supernova remnants: Application to Puppis A
title Rectangular core-collapse supernova remnants: Application to Puppis A
spellingShingle Rectangular core-collapse supernova remnants: Application to Puppis A
Meyer, D. M. A.
ISM: SUPERNOVA REMNANTS
METHODS: MHD
STARS: EVOLUTION
STARS: MASSIVE
title_short Rectangular core-collapse supernova remnants: Application to Puppis A
title_full Rectangular core-collapse supernova remnants: Application to Puppis A
title_fullStr Rectangular core-collapse supernova remnants: Application to Puppis A
title_full_unstemmed Rectangular core-collapse supernova remnants: Application to Puppis A
title_sort Rectangular core-collapse supernova remnants: Application to Puppis A
dc.creator.none.fl_str_mv Meyer, D. M. A.
Velázquez, Pablo F.
Petruk, Oleg
Chiotellis, Alexandros
Pohl, Michael
Camps Fariña, A.
Petrov, M.
Reynoso, Estela Marta
Toledo Roy, J. C.
Schneiter, Ernesto Matías
Castellanos Ramírez, A.
Esquivel, Alejandro
author Meyer, D. M. A.
author_facet Meyer, D. M. A.
Velázquez, Pablo F.
Petruk, Oleg
Chiotellis, Alexandros
Pohl, Michael
Camps Fariña, A.
Petrov, M.
Reynoso, Estela Marta
Toledo Roy, J. C.
Schneiter, Ernesto Matías
Castellanos Ramírez, A.
Esquivel, Alejandro
author_role author
author2 Velázquez, Pablo F.
Petruk, Oleg
Chiotellis, Alexandros
Pohl, Michael
Camps Fariña, A.
Petrov, M.
Reynoso, Estela Marta
Toledo Roy, J. C.
Schneiter, Ernesto Matías
Castellanos Ramírez, A.
Esquivel, Alejandro
author2_role author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ISM: SUPERNOVA REMNANTS
METHODS: MHD
STARS: EVOLUTION
STARS: MASSIVE
topic ISM: SUPERNOVA REMNANTS
METHODS: MHD
STARS: EVOLUTION
STARS: MASSIVE
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n ≈ 1 cm-3, T ≈ 8000 K), an organized magnetic field of strength 7μ G has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper, we show through 2.5D magnetohydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 M⊙ that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15-20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetized, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse-Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A.
Fil: Meyer, D. M. A.. Universitat Potsdam; Alemania
Fil: Velázquez, Pablo F.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Petruk, Oleg. No especifíca;
Fil: Chiotellis, Alexandros. National Observatory Of Athens; Grecia
Fil: Pohl, Michael. Universitat Potsdam; Alemania
Fil: Camps Fariña, A.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México. Universidad Complutense de Madrid; España
Fil: Petrov, M.. Max Planck Computing And Data Facility; Alemania
Fil: Reynoso, Estela Marta. Consejo Nacional de Investigaciones 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. Instituto de Ciencias Nucleares; México
Fil: Schneiter, Ernesto Matías. Universidad Nacional de Córdoba. Facultad de Cs.exactas Físicas y Naturales. Departamento de Materiales y Tecnología; Argentina
Fil: Castellanos Ramírez, A.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Esquivel, Alejandro. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
description Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n ≈ 1 cm-3, T ≈ 8000 K), an organized magnetic field of strength 7μ G has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper, we show through 2.5D magnetohydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 M⊙ that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15-20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetized, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse-Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A.
publishDate 2022
dc.date.none.fl_str_mv 2022-09
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/11336/216753
Meyer, D. M. A.; Velázquez, Pablo F.; Petruk, Oleg; Chiotellis, Alexandros; Pohl, Michael; et al.; Rectangular core-collapse supernova remnants: Application to Puppis A; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 515; 1; 9-2022; 594-605
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/216753
identifier_str_mv Meyer, D. M. A.; Velázquez, Pablo F.; Petruk, Oleg; Chiotellis, Alexandros; Pohl, Michael; et al.; Rectangular core-collapse supernova remnants: Application to Puppis A; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 515; 1; 9-2022; 594-605
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/515/1/594/6628661?redirectedFrom=fulltext
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac1832
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
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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 12.952241

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