Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh

Autores
Jerkstrand, A.; Ergon, M.; Smartt, S. J.; Fransson, C.; Sollerman, J.; Taubenberger, S.; Bersten, Melina Cecilia; Spyromilio, J.
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We investigate line formation processes in Type IIb supernovae (SNe) from 100 to 500 days post-explosion using spectral synthesis calculations. The modelling identifies the nuclear burning layers and physical mechanisms that produce the major emission lines, and the diagnostic potential of these. We compare the model calculations with data on the three best observed Type IIb SNe to-date − SN 1993J, SN 2008ax, and SN 2011dh. Oxygen nucleosynthesis depends sensitively on the main-sequence mass of the star and modelling of the [O I] λλ6300, 6364 lines constrains the progenitors of these three SNe to the MZAMS = 12−16 M range (ejected oxygen masses 0.3−0.9 M), with SN 2011dh towards the lower end and SN 1993J towards the upper end of the range. The high ejecta masses from MZAMS 17 M progenitors give rise to brighter nebular phase emission lines than observed. Nucleosynthesis analysis thus supports a scenario of low-to-moderate mass progenitors for Type IIb SNe, and by implication an origin in binary systems. We demonstrate how oxygen and magnesium recombination lines may be combined to diagnose the magnesium mass in the SN ejecta. For SN 2011dh, a magnesium mass of 0.02−0.14 M is derived, which gives a Mg/O production ratio consistent with the solar value. Nitrogen left in the He envelope from CNO burning gives strong [N II] λλ6548, 6583 emission lines that dominate over Hα emission in our models. The hydrogen envelopes of Type IIb SNe are too small and dilute to produce any noticeable Hα emission or absorption after ∼150 days, and nebular phase emission seen around 6550 Å is in many cases likely caused by [N II] λλ6548, 6583. Finally, the influence of radiative transport on the emergent line profiles is investigated. Significant line blocking in the metal core remains for several hundred days, which affects the emergent spectrum. These radiative transfer effects lead to early-time blueshifts of the emission line peaks, which gradually disappear as the optical depths decrease with time. The modelled evolution of this effect matches the observed evolution in SN 2011dh.
Fil: Jerkstrand, A.. The Queens University Of Belfast; Irlanda
Fil: Ergon, M. . Stockholms Universitet; Suecia
Fil: Smartt, S. J.. The Queens University Of Belfast; Irlanda
Fil: Fransson, C.. Stockholms Universitet; Suecia
Fil: Sollerman, J.. Stockholms Universitet; Suecia
Fil: Taubenberger, S.. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania
Fil: Bersten, Melina Cecilia. University of Tokyo; Japón. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Spyromilio, J.. European Southern Observatory; Alemania
Materia
RADIATIVETIVE TRANSFER
SN 2008ax
SN 2011dh
SN 1993J
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/10712
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/10712
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dhJerkstrand, A.Ergon, M. Smartt, S. J.Fransson, C.Sollerman, J.Taubenberger, S.Bersten, Melina CeciliaSpyromilio, J.RADIATIVETIVE TRANSFERSN 2008axSN 2011dhSN 1993Jhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We investigate line formation processes in Type IIb supernovae (SNe) from 100 to 500 days post-explosion using spectral synthesis calculations. The modelling identifies the nuclear burning layers and physical mechanisms that produce the major emission lines, and the diagnostic potential of these. We compare the model calculations with data on the three best observed Type IIb SNe to-date − SN 1993J, SN 2008ax, and SN 2011dh. Oxygen nucleosynthesis depends sensitively on the main-sequence mass of the star and modelling of the [O I] λλ6300, 6364 lines constrains the progenitors of these three SNe to the MZAMS = 12−16 M range (ejected oxygen masses 0.3−0.9 M), with SN 2011dh towards the lower end and SN 1993J towards the upper end of the range. The high ejecta masses from MZAMS 17 M progenitors give rise to brighter nebular phase emission lines than observed. Nucleosynthesis analysis thus supports a scenario of low-to-moderate mass progenitors for Type IIb SNe, and by implication an origin in binary systems. We demonstrate how oxygen and magnesium recombination lines may be combined to diagnose the magnesium mass in the SN ejecta. For SN 2011dh, a magnesium mass of 0.02−0.14 M is derived, which gives a Mg/O production ratio consistent with the solar value. Nitrogen left in the He envelope from CNO burning gives strong [N II] λλ6548, 6583 emission lines that dominate over Hα emission in our models. The hydrogen envelopes of Type IIb SNe are too small and dilute to produce any noticeable Hα emission or absorption after ∼150 days, and nebular phase emission seen around 6550 Å is in many cases likely caused by [N II] λλ6548, 6583. Finally, the influence of radiative transport on the emergent line profiles is investigated. Significant line blocking in the metal core remains for several hundred days, which affects the emergent spectrum. These radiative transfer effects lead to early-time blueshifts of the emission line peaks, which gradually disappear as the optical depths decrease with time. The modelled evolution of this effect matches the observed evolution in SN 2011dh.Fil: Jerkstrand, A.. The Queens University Of Belfast; IrlandaFil: Ergon, M. . Stockholms Universitet; SueciaFil: Smartt, S. J.. The Queens University Of Belfast; IrlandaFil: Fransson, C.. Stockholms Universitet; SueciaFil: Sollerman, J.. Stockholms Universitet; SueciaFil: Taubenberger, S.. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; AlemaniaFil: Bersten, Melina Cecilia. University of Tokyo; Japón. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Spyromilio, J.. European Southern Observatory; AlemaniaEdp Sciences2015-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/10712Jerkstrand, A.; Ergon, M. ; Smartt, S. J.; Fransson, C.; Sollerman, J.; et al.; Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh; Edp Sciences; Astronomy And Astrophysics; 573; 1-2015; 1-44; A120004-63611432-0746enginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201423983info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/01/aa23983-14/aa23983-14.htmlinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1408.0732info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:06:57Zoai:ri.conicet.gov.ar:11336/10712instacron: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:34982025-10-15 15:06:57.867CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
title Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
spellingShingle Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
Jerkstrand, A.
RADIATIVETIVE TRANSFER
SN 2008ax
SN 2011dh
SN 1993J
title_short Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
title_full Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
title_fullStr Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
title_full_unstemmed Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
title_sort Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh
dc.creator.none.fl_str_mv Jerkstrand, A.
Ergon, M.
Smartt, S. J.
Fransson, C.
Sollerman, J.
Taubenberger, S.
Bersten, Melina Cecilia
Spyromilio, J.
author Jerkstrand, A.
author_facet Jerkstrand, A.
Ergon, M.
Smartt, S. J.
Fransson, C.
Sollerman, J.
Taubenberger, S.
Bersten, Melina Cecilia
Spyromilio, J.
author_role author
author2 Ergon, M.
Smartt, S. J.
Fransson, C.
Sollerman, J.
Taubenberger, S.
Bersten, Melina Cecilia
Spyromilio, J.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv RADIATIVETIVE TRANSFER
SN 2008ax
SN 2011dh
SN 1993J
topic RADIATIVETIVE TRANSFER
SN 2008ax
SN 2011dh
SN 1993J
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 investigate line formation processes in Type IIb supernovae (SNe) from 100 to 500 days post-explosion using spectral synthesis calculations. The modelling identifies the nuclear burning layers and physical mechanisms that produce the major emission lines, and the diagnostic potential of these. We compare the model calculations with data on the three best observed Type IIb SNe to-date − SN 1993J, SN 2008ax, and SN 2011dh. Oxygen nucleosynthesis depends sensitively on the main-sequence mass of the star and modelling of the [O I] λλ6300, 6364 lines constrains the progenitors of these three SNe to the MZAMS = 12−16 M range (ejected oxygen masses 0.3−0.9 M), with SN 2011dh towards the lower end and SN 1993J towards the upper end of the range. The high ejecta masses from MZAMS 17 M progenitors give rise to brighter nebular phase emission lines than observed. Nucleosynthesis analysis thus supports a scenario of low-to-moderate mass progenitors for Type IIb SNe, and by implication an origin in binary systems. We demonstrate how oxygen and magnesium recombination lines may be combined to diagnose the magnesium mass in the SN ejecta. For SN 2011dh, a magnesium mass of 0.02−0.14 M is derived, which gives a Mg/O production ratio consistent with the solar value. Nitrogen left in the He envelope from CNO burning gives strong [N II] λλ6548, 6583 emission lines that dominate over Hα emission in our models. The hydrogen envelopes of Type IIb SNe are too small and dilute to produce any noticeable Hα emission or absorption after ∼150 days, and nebular phase emission seen around 6550 Å is in many cases likely caused by [N II] λλ6548, 6583. Finally, the influence of radiative transport on the emergent line profiles is investigated. Significant line blocking in the metal core remains for several hundred days, which affects the emergent spectrum. These radiative transfer effects lead to early-time blueshifts of the emission line peaks, which gradually disappear as the optical depths decrease with time. The modelled evolution of this effect matches the observed evolution in SN 2011dh.
Fil: Jerkstrand, A.. The Queens University Of Belfast; Irlanda
Fil: Ergon, M. . Stockholms Universitet; Suecia
Fil: Smartt, S. J.. The Queens University Of Belfast; Irlanda
Fil: Fransson, C.. Stockholms Universitet; Suecia
Fil: Sollerman, J.. Stockholms Universitet; Suecia
Fil: Taubenberger, S.. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania
Fil: Bersten, Melina Cecilia. University of Tokyo; Japón. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Spyromilio, J.. European Southern Observatory; Alemania
description We investigate line formation processes in Type IIb supernovae (SNe) from 100 to 500 days post-explosion using spectral synthesis calculations. The modelling identifies the nuclear burning layers and physical mechanisms that produce the major emission lines, and the diagnostic potential of these. We compare the model calculations with data on the three best observed Type IIb SNe to-date − SN 1993J, SN 2008ax, and SN 2011dh. Oxygen nucleosynthesis depends sensitively on the main-sequence mass of the star and modelling of the [O I] λλ6300, 6364 lines constrains the progenitors of these three SNe to the MZAMS = 12−16 M range (ejected oxygen masses 0.3−0.9 M), with SN 2011dh towards the lower end and SN 1993J towards the upper end of the range. The high ejecta masses from MZAMS 17 M progenitors give rise to brighter nebular phase emission lines than observed. Nucleosynthesis analysis thus supports a scenario of low-to-moderate mass progenitors for Type IIb SNe, and by implication an origin in binary systems. We demonstrate how oxygen and magnesium recombination lines may be combined to diagnose the magnesium mass in the SN ejecta. For SN 2011dh, a magnesium mass of 0.02−0.14 M is derived, which gives a Mg/O production ratio consistent with the solar value. Nitrogen left in the He envelope from CNO burning gives strong [N II] λλ6548, 6583 emission lines that dominate over Hα emission in our models. The hydrogen envelopes of Type IIb SNe are too small and dilute to produce any noticeable Hα emission or absorption after ∼150 days, and nebular phase emission seen around 6550 Å is in many cases likely caused by [N II] λλ6548, 6583. Finally, the influence of radiative transport on the emergent line profiles is investigated. Significant line blocking in the metal core remains for several hundred days, which affects the emergent spectrum. These radiative transfer effects lead to early-time blueshifts of the emission line peaks, which gradually disappear as the optical depths decrease with time. The modelled evolution of this effect matches the observed evolution in SN 2011dh.
publishDate 2015
dc.date.none.fl_str_mv 2015-01
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/11336/10712
Jerkstrand, A.; Ergon, M. ; Smartt, S. J.; Fransson, C.; Sollerman, J.; et al.; Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh; Edp Sciences; Astronomy And Astrophysics; 573; 1-2015; 1-44; A12
0004-6361
1432-0746
url http://hdl.handle.net/11336/10712
identifier_str_mv Jerkstrand, A.; Ergon, M. ; Smartt, S. J.; Fransson, C.; Sollerman, J.; et al.; Late-time spectral line formation in Type IIb supernovae, with application to SN 1993J, SN 2008ax, and SN 2011dh; Edp Sciences; Astronomy And Astrophysics; 573; 1-2015; 1-44; A12
0004-6361
1432-0746
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201423983
info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/01/aa23983-14/aa23983-14.html
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1408.0732
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Edp Sciences
publisher.none.fl_str_mv Edp Sciences
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
_version_ 1846083213127057408
score 13.221938

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