A 3D numerical model for Kepler's supernova remnant

Autores
Toledo Roy, J. C.; Esquivel, A.; Velazquez, P. F.; Reynoso, Estela Marta
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present new 3D numerical simulations for Kepler´s supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due to the large peculiar velocity of the system, the interaction of the strong AGB wind with the interstellar medium results in a bow shock structure. In this new model we propose that the AGB wind is anisotropic, with properties such as mass-loss rate and density having a latitude dependence, and that the orientation of the polar axis of the AGB star is not aligned with the direction of motion. The ejecta from the type Ia supernova explosion is modeled using a power-law density prole, and we let the remnant evolve for 400 yr. We computed synthetic X-ray maps from the numerical results. We find that the estimated size and peculiar X-ray morphology of Kepler´s SNR are well reproduced by considering an AGB mass-loss rate of 10-5 M_sol yr-1, a wind terminal velocity of 10 km s-1, an ambient medium density of 10-3 cm^3 and an explosion energy of 7x10^50 erg. The obtained total X-ray luminosity of the remnant in this model reaches 6x10^50 erg, which is within a factor of two of the observed value, and the time evolution of the luminosity shows a rate of decrease in recent decades of ~2.4% yr-1 that is consistent with the observations.
Fil: Toledo Roy, J. C.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Esquivel, A.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Velazquez, P. F.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Reynoso, Estela Marta. 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
Materia
methods: numerical
hydrodynamics
ISM: supernova remnants
radiation mechanisms: thermal
X-rays: ISM
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:11336/17374
Acceder
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repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling A 3D numerical model for Kepler's supernova remnantToledo Roy, J. C.Esquivel, A.Velazquez, P. F.Reynoso, Estela Martamethods: numericalhydrodynamicsISM: supernova remnantsradiation mechanisms: thermalX-rays: ISMhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present new 3D numerical simulations for Kepler´s supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due to the large peculiar velocity of the system, the interaction of the strong AGB wind with the interstellar medium results in a bow shock structure. In this new model we propose that the AGB wind is anisotropic, with properties such as mass-loss rate and density having a latitude dependence, and that the orientation of the polar axis of the AGB star is not aligned with the direction of motion. The ejecta from the type Ia supernova explosion is modeled using a power-law density prole, and we let the remnant evolve for 400 yr. We computed synthetic X-ray maps from the numerical results. We find that the estimated size and peculiar X-ray morphology of Kepler´s SNR are well reproduced by considering an AGB mass-loss rate of 10-5 M_sol yr-1, a wind terminal velocity of 10 km s-1, an ambient medium density of 10-3 cm^3 and an explosion energy of 7x10^50 erg. The obtained total X-ray luminosity of the remnant in this model reaches 6x10^50 erg, which is within a factor of two of the observed value, and the time evolution of the luminosity shows a rate of decrease in recent decades of ~2.4% yr-1 that is consistent with the observations.Fil: Toledo Roy, J. C.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; MéxicoFil: Esquivel, A.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; MéxicoFil: Velazquez, P. F.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; MéxicoFil: Reynoso, Estela Marta. 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; ArgentinaOxford University Press2014-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/17374Toledo Roy, J. C.; Esquivel, A.; Velazquez, P. F.; Reynoso, Estela Marta; A 3D numerical model for Kepler's supernova remnant; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 442; 1; 5-2014; 229-2380035-8711enginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stu880info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/442/1/229/1247978/A-3D-numerical-model-for-Kepler-s-supernova?redirectedFrom=fulltextinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:22:05Zoai:ri.conicet.gov.ar:11336/17374instacron: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 10:22:05.759CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A 3D numerical model for Kepler's supernova remnant
title A 3D numerical model for Kepler's supernova remnant
spellingShingle A 3D numerical model for Kepler's supernova remnant
Toledo Roy, J. C.
methods: numerical
hydrodynamics
ISM: supernova remnants
radiation mechanisms: thermal
X-rays: ISM
title_short A 3D numerical model for Kepler's supernova remnant
title_full A 3D numerical model for Kepler's supernova remnant
title_fullStr A 3D numerical model for Kepler's supernova remnant
title_full_unstemmed A 3D numerical model for Kepler's supernova remnant
title_sort A 3D numerical model for Kepler's supernova remnant
dc.creator.none.fl_str_mv Toledo Roy, J. C.
Esquivel, A.
Velazquez, P. F.
Reynoso, Estela Marta
author Toledo Roy, J. C.
author_facet Toledo Roy, J. C.
Esquivel, A.
Velazquez, P. F.
Reynoso, Estela Marta
author_role author
author2 Esquivel, A.
Velazquez, P. F.
Reynoso, Estela Marta
author2_role author
author
author
dc.subject.none.fl_str_mv methods: numerical
hydrodynamics
ISM: supernova remnants
radiation mechanisms: thermal
X-rays: ISM
topic methods: numerical
hydrodynamics
ISM: supernova remnants
radiation mechanisms: thermal
X-rays: ISM
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present new 3D numerical simulations for Kepler´s supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due to the large peculiar velocity of the system, the interaction of the strong AGB wind with the interstellar medium results in a bow shock structure. In this new model we propose that the AGB wind is anisotropic, with properties such as mass-loss rate and density having a latitude dependence, and that the orientation of the polar axis of the AGB star is not aligned with the direction of motion. The ejecta from the type Ia supernova explosion is modeled using a power-law density prole, and we let the remnant evolve for 400 yr. We computed synthetic X-ray maps from the numerical results. We find that the estimated size and peculiar X-ray morphology of Kepler´s SNR are well reproduced by considering an AGB mass-loss rate of 10-5 M_sol yr-1, a wind terminal velocity of 10 km s-1, an ambient medium density of 10-3 cm^3 and an explosion energy of 7x10^50 erg. The obtained total X-ray luminosity of the remnant in this model reaches 6x10^50 erg, which is within a factor of two of the observed value, and the time evolution of the luminosity shows a rate of decrease in recent decades of ~2.4% yr-1 that is consistent with the observations.
Fil: Toledo Roy, J. C.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Esquivel, A.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Velazquez, P. F.. Universidad Nacional Autónoma de México. Instituto de Ciencias Nucleares; México
Fil: Reynoso, Estela Marta. 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
description We present new 3D numerical simulations for Kepler´s supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due to the large peculiar velocity of the system, the interaction of the strong AGB wind with the interstellar medium results in a bow shock structure. In this new model we propose that the AGB wind is anisotropic, with properties such as mass-loss rate and density having a latitude dependence, and that the orientation of the polar axis of the AGB star is not aligned with the direction of motion. The ejecta from the type Ia supernova explosion is modeled using a power-law density prole, and we let the remnant evolve for 400 yr. We computed synthetic X-ray maps from the numerical results. We find that the estimated size and peculiar X-ray morphology of Kepler´s SNR are well reproduced by considering an AGB mass-loss rate of 10-5 M_sol yr-1, a wind terminal velocity of 10 km s-1, an ambient medium density of 10-3 cm^3 and an explosion energy of 7x10^50 erg. The obtained total X-ray luminosity of the remnant in this model reaches 6x10^50 erg, which is within a factor of two of the observed value, and the time evolution of the luminosity shows a rate of decrease in recent decades of ~2.4% yr-1 that is consistent with the observations.
publishDate 2014
dc.date.none.fl_str_mv 2014-05
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/11336/17374
Toledo Roy, J. C.; Esquivel, A.; Velazquez, P. F.; Reynoso, Estela Marta; A 3D numerical model for Kepler's supernova remnant; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 442; 1; 5-2014; 229-238
0035-8711
url http://hdl.handle.net/11336/17374
identifier_str_mv Toledo Roy, J. C.; Esquivel, A.; Velazquez, P. F.; Reynoso, Estela Marta; A 3D numerical model for Kepler's supernova remnant; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 442; 1; 5-2014; 229-238
0035-8711
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stu880
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/442/1/229/1247978/A-3D-numerical-model-for-Kepler-s-supernova?redirectedFrom=fulltext
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 13.070432

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