Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies

We perform hydrodynamical simulations of the interaction between supernova (SN) ejecta and circumstellar medium (CSM) for SN 1993J and SN 2011dh, and calculate the radio and X-ray emissions expected from the shocked gas at late epochs (t). Considering the ejecta structure from multi-group radiation...

Descripción completa

Detalles Bibliográficos
Autores: Kundu, E., Lundqvist, P., Sorokina, E., Pérez-Torres, Miguel A., Blinnikov, S., O'connor, E., Ergon, M., Chandra, P., Das, B.
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2019
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/193950
Acceso en línea:http://hdl.handle.net/10261/193950
Access Level:acceso abierto
Palabra clave:Supernovae: Individual (SN 1993J, SN 2011dh
Radiation Mechanisms: Thermal
Radiation Mechanisms: non-Thermal
Hydrodynamics
Circumstellar matter
id ES_d90666732ecaeab34efb4e58dbc4ab93
oai_identifier_str oai:digital.csic.es:10261/193950
network_acronym_str ES
network_name_str España
repository_id_str
spelling Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray StudiesKundu, E.Lundqvist, P.Sorokina, E.Pérez-Torres, Miguel A.Blinnikov, S.O'connor, E.Ergon, M.Chandra, P.Das, B.Supernovae: Individual (SN 1993J, SN 2011dhRadiation Mechanisms: ThermalRadiation Mechanisms: non-ThermalHydrodynamicsCircumstellar matterWe perform hydrodynamical simulations of the interaction between supernova (SN) ejecta and circumstellar medium (CSM) for SN 1993J and SN 2011dh, and calculate the radio and X-ray emissions expected from the shocked gas at late epochs (t). Considering the ejecta structure from multi-group radiation hydrodynamics simulation, we find that the observed rapid drop in radio and X-ray light curves of SN 1993J at t > 3000 days may be due to a change in the mass-loss rate () ∼6500 yr prior to the explosion of the SN. The exact epoch scales inversely with the assumed wind velocity of v = 10 . The progenitor of this SN very likely belonged to a binary system, where, during its evolution, the primary had transferred material to the secondary. It is argued in this paper that the change in can happen because of a change in the mass accretion efficiency (η) of the companion star. It is possible that before ∼6500 (v/10 ) yr prior to the explosion, η was high, and thus the CSM was tenuous, which causes the late-time downturn in fluxes. In the case of SN 2011dh, the late-time evolution is found to be consistent with a wind medium with/v = 4 × 10/10 . It is difficult from our analysis to predict whether the progenitor of this SN had a binary companion; however, if future observations show a similar decrease in radio and X-ray fluxes, then this would give strong support to a scenario where both SNe had undergone a similar kind of binary evolution before explosion.© 2019. The American Astronomical Society. All rights reserved.Peer ReviewedIOP PublishingConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2019201920192019info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/193950reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttp://dx.doi.org/10.3847/1538-4357/ab0d81Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/1939502026-05-22T06:33:51Z
dc.title.none.fl_str_mv Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
title Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
spellingShingle Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
Kundu, E.
Supernovae: Individual (SN 1993J, SN 2011dh
Radiation Mechanisms: Thermal
Radiation Mechanisms: non-Thermal
Hydrodynamics
Circumstellar matter
title_short Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
title_full Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
title_fullStr Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
title_full_unstemmed Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
title_sort Evolution of the Progenitors of SNe 1993J and 2011dh Revealed through Late-time Radio and X-Ray Studies
dc.creator.none.fl_str_mv Kundu, E.
Lundqvist, P.
Sorokina, E.
Pérez-Torres, Miguel A.
Blinnikov, S.
O'connor, E.
Ergon, M.
Chandra, P.
Das, B.
author Kundu, E.
author_facet Kundu, E.
Lundqvist, P.
Sorokina, E.
Pérez-Torres, Miguel A.
Blinnikov, S.
O'connor, E.
Ergon, M.
Chandra, P.
Das, B.
author_role author
author2 Lundqvist, P.
Sorokina, E.
Pérez-Torres, Miguel A.
Blinnikov, S.
O'connor, E.
Ergon, M.
Chandra, P.
Das, B.
author2_role author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Supernovae: Individual (SN 1993J, SN 2011dh
Radiation Mechanisms: Thermal
Radiation Mechanisms: non-Thermal
Hydrodynamics
Circumstellar matter
topic Supernovae: Individual (SN 1993J, SN 2011dh
Radiation Mechanisms: Thermal
Radiation Mechanisms: non-Thermal
Hydrodynamics
Circumstellar matter
description We perform hydrodynamical simulations of the interaction between supernova (SN) ejecta and circumstellar medium (CSM) for SN 1993J and SN 2011dh, and calculate the radio and X-ray emissions expected from the shocked gas at late epochs (t). Considering the ejecta structure from multi-group radiation hydrodynamics simulation, we find that the observed rapid drop in radio and X-ray light curves of SN 1993J at t > 3000 days may be due to a change in the mass-loss rate () ∼6500 yr prior to the explosion of the SN. The exact epoch scales inversely with the assumed wind velocity of v = 10 . The progenitor of this SN very likely belonged to a binary system, where, during its evolution, the primary had transferred material to the secondary. It is argued in this paper that the change in can happen because of a change in the mass accretion efficiency (η) of the companion star. It is possible that before ∼6500 (v/10 ) yr prior to the explosion, η was high, and thus the CSM was tenuous, which causes the late-time downturn in fluxes. In the case of SN 2011dh, the late-time evolution is found to be consistent with a wind medium with/v = 4 × 10/10 . It is difficult from our analysis to predict whether the progenitor of this SN had a binary companion; however, if future observations show a similar decrease in radio and X-ray fluxes, then this would give strong support to a scenario where both SNe had undergone a similar kind of binary evolution before explosion.© 2019. The American Astronomical Society. All rights reserved.
publishDate 2019
dc.date.none.fl_str_mv 2019
2019
2019
2019
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Postprint
info:eu-repo/semantics/acceptedVersion
format article
status_str acceptedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/193950
url http://hdl.handle.net/10261/193950
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv http://dx.doi.org/10.3847/1538-4357/ab0d81
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869421276775317504
score 15,811543

Similares en LA Referencia