Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754

The beginning of photoionization marks the transition between the post-AGB and planetary nebula (PN) phases of stars with masses ≲ 8 M ⊙ . This critical phase is difficult to observe, as it lasts only a few decades. The combination of jets and magnetic fields, the key agents of PN?shaping, could giv...

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Autores: Suárez, Olga, Gómez, José F., Bendjoya, Philippe, Miranda, Luis F., Guerrero, Martín A., Uscanga, Lucero, Green, James A., Rizzo, J. Ricardo, Ramos-Larios, Gerardo
Formato: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2015
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/398004
Acesso em linha:http://hdl.handle.net/10261/398004
Access Level:acceso abierto
Palavra-chave:Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103–5754)
Radio continuum: stars
Stars: AGB and post-AGB
Stars: magnetic field
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spelling Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754Suárez, OlgaGómez, José F.Bendjoya, PhilippeMiranda, Luis F.Guerrero, Martín A.Uscanga, LuceroGreen, James A.Rizzo, J. RicardoRamos-Larios, GerardoPlanetary nebulae: generalPlanetary nebulae: individual (IRAS 15103–5754)Radio continuum: starsStars: AGB and post-AGBStars: magnetic fieldThe beginning of photoionization marks the transition between the post-AGB and planetary nebula (PN) phases of stars with masses ≲ 8 M ⊙ . This critical phase is difficult to observe, as it lasts only a few decades. The combination of jets and magnetic fields, the key agents of PN?shaping, could give rise to synchrotron emission, but this has never been observed before in any PNe, since freefree emission from the ionized gas is expected to dominate its radio spectrum. In this paper we report radio continuum observations taken with the ATCA between 1 and 46 GHz of the young PN IRAS 151035754. Our observations in 20102011 show non-thermal emission compatible with synchrotron emission from electrons accelerated at a shock with spectral index a α -0.54. However, in 2012, the spectral index a ≃ -0.28 is no longer compatible with synchrotron emission in these types of processes. Several hypotheses are discussed to explain this change. The more plausible ones are related to the presence of the newly photoionized region in this young PN: either energy loss of electrons due to Coulomb collisions with the plasma, or selective suppression of synchrotron radiation due to the Razin effect. We postulate that the observed flattening of non-thermal radio spectra could be a hallmark identifying the beginning of the PN phase. © 2015. The American Astronomical Society. All rights reserved.The authors acknowledge financial support from MICINN (Spain) grants AYA2011-29754-C03-02, AYA2011-30228-C03 (both including FEDER funds), CSD2009-00038, AYA2009-07304, and AYA2012-32032, from grant PE9-1160 of the Greek General Secretariat for Research and Technology, from CONACyT and PROMEP (Mexico), from Ministerio de Educación (Spain) under Programa Nacional de Movilidad de Recursos Humanos del Plan Nacional de I+D+I 2008–2011.Peer reviewedIOP PublishingMinisterio de Ciencia e Innovación (España)European CommissionComisión Nacional de Investigación Científica y Tecnológica (Chile)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252015info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/398004reponame: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/MICINN//AYA2011-29754-C03-02info:eu-repo/grantAgreement/MICINN//AYA2011-30228-C03info:eu-repo/grantAgreement/MICINN//CSD2009-00038info:eu-repo/grantAgreement/MICINN//AYA2009-07304info:eu-repo/grantAgreement/MINECO//AYA2012-32032http://dx.doi.org/10.1088/0004-637X/806/1/105Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3980042026-05-22T06:33:51Z
dc.title.none.fl_str_mv Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
title Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
spellingShingle Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
Suárez, Olga
Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103–5754)
Radio continuum: stars
Stars: AGB and post-AGB
Stars: magnetic field
title_short Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
title_full Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
title_fullStr Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
title_full_unstemmed Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
title_sort Time-variable Non-thermal Emission in the Planetary Nebula IRAS 15103-5754
dc.creator.none.fl_str_mv Suárez, Olga
Gómez, José F.
Bendjoya, Philippe
Miranda, Luis F.
Guerrero, Martín A.
Uscanga, Lucero
Green, James A.
Rizzo, J. Ricardo
Ramos-Larios, Gerardo
author Suárez, Olga
author_facet Suárez, Olga
Gómez, José F.
Bendjoya, Philippe
Miranda, Luis F.
Guerrero, Martín A.
Uscanga, Lucero
Green, James A.
Rizzo, J. Ricardo
Ramos-Larios, Gerardo
author_role author
author2 Gómez, José F.
Bendjoya, Philippe
Miranda, Luis F.
Guerrero, Martín A.
Uscanga, Lucero
Green, James A.
Rizzo, J. Ricardo
Ramos-Larios, Gerardo
author2_role author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
European Commission
Comisión Nacional de Investigación Científica y Tecnológica (Chile)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103–5754)
Radio continuum: stars
Stars: AGB and post-AGB
Stars: magnetic field
topic Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103–5754)
Radio continuum: stars
Stars: AGB and post-AGB
Stars: magnetic field
description The beginning of photoionization marks the transition between the post-AGB and planetary nebula (PN) phases of stars with masses ≲ 8 M ⊙ . This critical phase is difficult to observe, as it lasts only a few decades. The combination of jets and magnetic fields, the key agents of PN?shaping, could give rise to synchrotron emission, but this has never been observed before in any PNe, since freefree emission from the ionized gas is expected to dominate its radio spectrum. In this paper we report radio continuum observations taken with the ATCA between 1 and 46 GHz of the young PN IRAS 151035754. Our observations in 20102011 show non-thermal emission compatible with synchrotron emission from electrons accelerated at a shock with spectral index a α -0.54. However, in 2012, the spectral index a ≃ -0.28 is no longer compatible with synchrotron emission in these types of processes. Several hypotheses are discussed to explain this change. The more plausible ones are related to the presence of the newly photoionized region in this young PN: either energy loss of electrons due to Coulomb collisions with the plasma, or selective suppression of synchrotron radiation due to the Razin effect. We postulate that the observed flattening of non-thermal radio spectra could be a hallmark identifying the beginning of the PN phase. © 2015. The American Astronomical Society. All rights reserved.
publishDate 2015
dc.date.none.fl_str_mv 2015
2025
2025
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/10261/398004
url http://hdl.handle.net/10261/398004
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MICINN//AYA2011-29754-C03-02
info:eu-repo/grantAgreement/MICINN//AYA2011-30228-C03
info:eu-repo/grantAgreement/MICINN//CSD2009-00038
info:eu-repo/grantAgreement/MICINN//AYA2009-07304
info:eu-repo/grantAgreement/MINECO//AYA2012-32032
http://dx.doi.org/10.1088/0004-637X/806/1/105
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
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score 15,81155

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