The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability
Context. Observations of radio emission from young core-collapse supernovae (CCSNe) allow one to study the history of the pre-supernova stellar wind, trace the density structure of the ejected material, and probe the magnetohydrodynamics that describe the interaction between the two, as the forward...
| Autores: | , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/373100 |
| Acceso en línea: | http://hdl.handle.net/10261/373100 |
| Access Level: | acceso abierto |
| Palabra clave: | Radiation mechanisms: non-thermal Supernovae: general ISM: supernova remnants Supernovae: individual: SN 1993J |
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España |
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| dc.title.none.fl_str_mv |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability |
| title |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability |
| spellingShingle |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability Martí-Vidal, Iván Radiation mechanisms: non-thermal Supernovae: general ISM: supernova remnants Supernovae: individual: SN 1993J |
| title_short |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability |
| title_full |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability |
| title_fullStr |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability |
| title_full_unstemmed |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability |
| title_sort |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instability |
| dc.creator.none.fl_str_mv |
Martí-Vidal, Iván Björnsson, Claes-Ingvar Pérez-Torres, Miguel A. Lundqvist, P. Marcaide, J.M. |
| author |
Martí-Vidal, Iván |
| author_facet |
Martí-Vidal, Iván Björnsson, Claes-Ingvar Pérez-Torres, Miguel A. Lundqvist, P. Marcaide, J.M. |
| author_role |
author |
| author2 |
Björnsson, Claes-Ingvar Pérez-Torres, Miguel A. Lundqvist, P. Marcaide, J.M. |
| author2_role |
author author author author |
| dc.contributor.none.fl_str_mv |
Generalitat Valenciana Ministerio de Ciencia e Innovación (España) European Commission Ministerio de Ciencia, Innovación y Universidades (España) Agencia Estatal de Investigación (España) Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Radiation mechanisms: non-thermal Supernovae: general ISM: supernova remnants Supernovae: individual: SN 1993J |
| topic |
Radiation mechanisms: non-thermal Supernovae: general ISM: supernova remnants Supernovae: individual: SN 1993J |
| description |
Context. Observations of radio emission from young core-collapse supernovae (CCSNe) allow one to study the history of the pre-supernova stellar wind, trace the density structure of the ejected material, and probe the magnetohydrodynamics that describe the interaction between the two, as the forward shock expands into the circumstellar medium. The radio shell of supernova SN 1993J has been observed with very long baseline interferometry (VLBI) for ∼20 years, giving one of the most complete pictures of the evolution of a CCSN shock. However, different results about the expansion curve and properties of the radio-emitting structure have been reported by different authors, likely due to systematics in the data calibration and/or model assumptions made by each team. |
| publishDate |
2024 |
| dc.date.none.fl_str_mv |
2024 2024 2024 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/373100 |
| url |
http://hdl.handle.net/10261/373100 |
| dc.language.none.fl_str_mv |
Inglés |
| language_invalid_str_mv |
Inglés |
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#PLACEHOLDER_PARENT_METADATA_VALUE# #PLACEHOLDER_PARENT_METADATA_VALUE# #PLACEHOLDER_PARENT_METADATA_VALUE# #PLACEHOLDER_PARENT_METADATA_VALUE# #PLACEHOLDER_PARENT_METADATA_VALUE# info:eu-repo/grantAgreement/AEI//CIDEGENT info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-108995GB-C22 info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2022-140888NB-C22 info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-117404GB-C21 info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2021-001131-S http://dx.doi.org/10.1051/0004-6361/202450329 Sí |
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info:eu-repo/semantics/openAccess |
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openAccess |
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European Southern Observatory |
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European Southern Observatory |
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reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
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Consejo Superior de Investigaciones Científicas (CSIC) |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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1869403352783126528 |
| spelling |
The radial distribution of radio emission from SN 1993J: Magnetic field amplification due to the Rayleigh-Taylor instabilityMartí-Vidal, IvánBjörnsson, Claes-IngvarPérez-Torres, Miguel A.Lundqvist, P.Marcaide, J.M.Radiation mechanisms: non-thermalSupernovae: generalISM: supernova remnantsSupernovae: individual: SN 1993JContext. Observations of radio emission from young core-collapse supernovae (CCSNe) allow one to study the history of the pre-supernova stellar wind, trace the density structure of the ejected material, and probe the magnetohydrodynamics that describe the interaction between the two, as the forward shock expands into the circumstellar medium. The radio shell of supernova SN 1993J has been observed with very long baseline interferometry (VLBI) for ∼20 years, giving one of the most complete pictures of the evolution of a CCSN shock. However, different results about the expansion curve and properties of the radio-emitting structure have been reported by different authors, likely due to systematics in the data calibration and/or model assumptions made by each team.Aims. We aim to perform an analysis of the complete set of VLBI observations of SN 1993J that accounts for different instrumental and source-intrinsic effects, in order to retrieve robust conclusions about the shock expansion and physics in SN 1993J.Methods. We have explored the posterior probability distribution of a complete data model, using a technique based on Markov chains. Our model accounts for antenna calibration effects, as well as different kinds of radio-emission structures for the supernova.Results. The posterior parameter distributions strongly favor a spherical shell-like radio structure with a nonuniform radial intensity profile, with a broad brightness distribution that peaks close to or just above the region where the contact discontinuity is expected to be located. Regarding the shell expansion, the full dataset can be well described using one single deceleration parameter, β ∼ 0.80, being the shell outer radius R ∝ tβ. There is clear evidence of a relative widening of the shell width beyond day 2600−3300 after the explosion, which is due to an increased deceleration of the inner shell boundary. This is similar to findings previously reported by other authors.Conclusions. The radial intensity profile and the late evolution of the shell suggest a scenario in which the magnetic field is amplified mainly by the Rayleigh-Taylor instability, which emanates from the contact discontinuity. Furthermore, the increased deceleration of the inner boundary indicates that the reverse shock enters a region of the ejecta at around 3000 days, where the density distribution is substantially flatter. Such a weakening of the reverse shock can also explain the achromatic break in the radio light curves, which occurs at the same time. The deduced radial intensity distribution for SN 1993J is quite similar to that observed in the spatially well-resolved supernova remnant Cassiopeia A.This work has been partially supported by the Generalitat Valenciana GenT Project CIDEGENT/2018/021 and by the MICINN Research Projects PID2019-108995GB-C22 and PID2022-140888NB-C22. IMV acknowledges support from the Astrophysics and High Energy Physics programme by MCIN, with funding from European Union NextGenerationEU (PRTR-C17I1) and the Generalitat Valenciana through grant ASFAE/2022/018. MPT acknowledges financial support from the Severo Ochoa grant CEX2021- 001131-S and from the National grant PID2020-117404GB-C21, funded by MCIU/AEI/10.13039/501100011033.Peer reviewedEuropean Southern ObservatoryGeneralitat ValencianaMinisterio de Ciencia e Innovación (España)European CommissionMinisterio de Ciencia, Innovación y Universidades (España)Agencia Estatal de Investigación (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202420242024info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/373100reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI//CIDEGENTinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-108995GB-C22info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2022-140888NB-C22info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-117404GB-C21info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2021-001131-Shttp://dx.doi.org/10.1051/0004-6361/202450329Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3731002026-05-22T06:33:51Z |
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