Early ultraviolet/optical emission of the type Ib SN 2008D

We propose an alternative explanation for the post-breakout emission of SN 2008D associated with the X-ray transient 080109. Observations of this object show a very small contrast of 0.35 dex between the light-curve minimum occurring soon after the breakout, and the main luminosity peak which is due...

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Autores: Bersten, Melina Cecilia, Tanaka, Masaomi, Tominaga, Nozomu, Benvenuto, Omar Gustavo, Nomoto, Ken’ichi
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2013
País:Argentina
Institución:Universidad Nacional de La Plata
Repositorio:SEDICI (UNLP)
Idioma:inglés
OAI Identifier:oai:sedici.unlp.edu.ar:10915/85483
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/85483
Access Level:acceso abierto
Palabra clave:Ciencias Astronómicas
hydrodynamics
supernovae: general
supernovae: individual (SN 2008D)
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spelling Early ultraviolet/optical emission of the type Ib SN 2008DBersten, Melina CeciliaTanaka, MasaomiTominaga, NozomuBenvenuto, Omar GustavoNomoto, Ken’ichiCiencias Astronómicashydrodynamicssupernovae: generalsupernovae: individual (SN 2008D)We propose an alternative explanation for the post-breakout emission of SN 2008D associated with the X-ray transient 080109. Observations of this object show a very small contrast of 0.35 dex between the light-curve minimum occurring soon after the breakout, and the main luminosity peak which is due to radioactive heating of the ejecta. Hydrodynamical models show that the cooling of a shocked Wolf-Rayet star leads to a much greater difference (≳ 0.9 dex). Our proposed scenario is that of a jet produced during the explosion which deposits 56Ni-rich material in the outer layers of the ejecta. The presence of high-velocity radioactive material allows us to reproduce the complete luminosity evolution of the object. Without outer 56Ni it could be possible to reproduce the early emission purely from cooling of the shocked envelope by assuming a larger progenitor than a Wolf-Rayet star, but that would require an initial density structure significantly different from what is predicted by stellar evolution models. Analytic models of the cooling phase have been proposed reproduce the early emission of SN 2008D with an extended progenitor. However, we found that the models are valid only until 1.5 days after the explosion where only two data of SN 2008D are available. We also discuss the possibility of the interaction of the ejecta with a binary companion, based on published analytic expressions. However, the binary separation required to fit the early emission should be ≲ 3 R ⊙, which is too small for a system containing two massive stars.Facultad de Ciencias Astronómicas y Geofísicas2013info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/85483enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/767/2/143info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2024-05-08T12:54:32Zoai:sedici.unlp.edu.ar:10915/85483Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292024-05-08 12:54:33.151SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Early ultraviolet/optical emission of the type Ib SN 2008D
title Early ultraviolet/optical emission of the type Ib SN 2008D
spellingShingle Early ultraviolet/optical emission of the type Ib SN 2008D
Bersten, Melina Cecilia
Ciencias Astronómicas
hydrodynamics
supernovae: general
supernovae: individual (SN 2008D)
title_short Early ultraviolet/optical emission of the type Ib SN 2008D
title_full Early ultraviolet/optical emission of the type Ib SN 2008D
title_fullStr Early ultraviolet/optical emission of the type Ib SN 2008D
title_full_unstemmed Early ultraviolet/optical emission of the type Ib SN 2008D
title_sort Early ultraviolet/optical emission of the type Ib SN 2008D
dc.creator.none.fl_str_mv Bersten, Melina Cecilia
Tanaka, Masaomi
Tominaga, Nozomu
Benvenuto, Omar Gustavo
Nomoto, Ken’ichi
author Bersten, Melina Cecilia
author_facet Bersten, Melina Cecilia
Tanaka, Masaomi
Tominaga, Nozomu
Benvenuto, Omar Gustavo
Nomoto, Ken’ichi
author_role author
author2 Tanaka, Masaomi
Tominaga, Nozomu
Benvenuto, Omar Gustavo
Nomoto, Ken’ichi
author2_role author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
hydrodynamics
supernovae: general
supernovae: individual (SN 2008D)
topic Ciencias Astronómicas
hydrodynamics
supernovae: general
supernovae: individual (SN 2008D)
description We propose an alternative explanation for the post-breakout emission of SN 2008D associated with the X-ray transient 080109. Observations of this object show a very small contrast of 0.35 dex between the light-curve minimum occurring soon after the breakout, and the main luminosity peak which is due to radioactive heating of the ejecta. Hydrodynamical models show that the cooling of a shocked Wolf-Rayet star leads to a much greater difference (≳ 0.9 dex). Our proposed scenario is that of a jet produced during the explosion which deposits 56Ni-rich material in the outer layers of the ejecta. The presence of high-velocity radioactive material allows us to reproduce the complete luminosity evolution of the object. Without outer 56Ni it could be possible to reproduce the early emission purely from cooling of the shocked envelope by assuming a larger progenitor than a Wolf-Rayet star, but that would require an initial density structure significantly different from what is predicted by stellar evolution models. Analytic models of the cooling phase have been proposed reproduce the early emission of SN 2008D with an extended progenitor. However, we found that the models are valid only until 1.5 days after the explosion where only two data of SN 2008D are available. We also discuss the possibility of the interaction of the ejecta with a binary companion, based on published analytic expressions. However, the binary separation required to fit the early emission should be ≲ 3 R ⊙, which is too small for a system containing two massive stars.
publishDate 2013
dc.date.none.fl_str_mv 2013
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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://sedici.unlp.edu.ar/handle/10915/85483
url http://sedici.unlp.edu.ar/handle/10915/85483
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-637X
info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/767/2/143
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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score 15,81155

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