Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations

Autores
Blanco, A. B.; De Becker, M.; Saha, A.; Tej, A.; Benaglia, Paula
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Massive stars produce strong stellar winds that consist of continuous outflows of material at speeds of thousands of km s‑1. These winds convey large amounts of kinetic power, especially in the case of Wolf–Rayet (WR) stars. When these winds interact with nearby material, they will likely produce shocks. Among other processes, particle acceleration is expected to occur. This is particularly well established in the case of massive binary systems, where the stellar winds collide, allowing these systems to be identified thanks to the detection of synchrotron radio emission, produced by a population of relativistic particles accelerated in the shocks. Aims. Our goal is to investigate the occurrence of particle acceleration among massive stars in their pre-supernova evolution phases. Methods. We observed a subset of five WR stars in the radio domain using the upgraded Giant Metrewave Radio Telescope (uGMRT), located in India. The observations were carried out in bands 4 (550–950 MHz) and 5 (1050–1450 MHz) for all the targets. Results. We detected radio emission for only WR 110 in bands 4 and 5. Its thermal spectrum displays a consistent index of +0.74 down to uGMRT bands. The four other targets were not detected and we derived 3σ upper limits on their flux density. Our upper limits in Band 4 are the first provided for these targets below 1 GHz. None of the targets was identified as a synchrotron radio emitter in these radio bands. Conclusions. If some synchrotron emission is produced in these systems, the non-detection with the uGMRT can be most likely attributed to strong free-free absorption (FFA). This is especially relevant for WR98a which is catalogued as a particle accelerator based on previous measurements at higher radio frequencies. The prominence of FFA constitutes a severe obstacle to identifying particle accelerators in the radio domain.
Fil: Blanco, A. B.. Université de Liège; Bélgica
Fil: De Becker, M.. Université de Liège; Bélgica
Fil: Saha, A.. Indian Institute Of Space Science And Technology; India
Fil: Tej, A.. Indian Institute Of Space Science And Technology; India
Fil: Benaglia, Paula. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Materia
ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERRMAL
STARS: WOLF RAYET
RADIO CONTINUUM:STARS
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:11336/261355
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/261355
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observationsBlanco, A. B.De Becker, M.Saha, A.Tej, A.Benaglia, PaulaACCELERATION OF PARTICLESRADIATION MECHANISMS: NON-THERRMALSTARS: WOLF RAYETRADIO CONTINUUM:STARShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Massive stars produce strong stellar winds that consist of continuous outflows of material at speeds of thousands of km s‑1. These winds convey large amounts of kinetic power, especially in the case of Wolf–Rayet (WR) stars. When these winds interact with nearby material, they will likely produce shocks. Among other processes, particle acceleration is expected to occur. This is particularly well established in the case of massive binary systems, where the stellar winds collide, allowing these systems to be identified thanks to the detection of synchrotron radio emission, produced by a population of relativistic particles accelerated in the shocks. Aims. Our goal is to investigate the occurrence of particle acceleration among massive stars in their pre-supernova evolution phases. Methods. We observed a subset of five WR stars in the radio domain using the upgraded Giant Metrewave Radio Telescope (uGMRT), located in India. The observations were carried out in bands 4 (550–950 MHz) and 5 (1050–1450 MHz) for all the targets. Results. We detected radio emission for only WR 110 in bands 4 and 5. Its thermal spectrum displays a consistent index of +0.74 down to uGMRT bands. The four other targets were not detected and we derived 3σ upper limits on their flux density. Our upper limits in Band 4 are the first provided for these targets below 1 GHz. None of the targets was identified as a synchrotron radio emitter in these radio bands. Conclusions. If some synchrotron emission is produced in these systems, the non-detection with the uGMRT can be most likely attributed to strong free-free absorption (FFA). This is especially relevant for WR98a which is catalogued as a particle accelerator based on previous measurements at higher radio frequencies. The prominence of FFA constitutes a severe obstacle to identifying particle accelerators in the radio domain.Fil: Blanco, A. B.. Université de Liège; BélgicaFil: De Becker, M.. Université de Liège; BélgicaFil: Saha, A.. Indian Institute Of Space Science And Technology; IndiaFil: Tej, A.. Indian Institute Of Space Science And Technology; IndiaFil: Benaglia, Paula. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaEDP Sciences2024-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/261355Blanco, A. B.; De Becker, M.; Saha, A.; Tej, A.; Benaglia, Paula; Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations; EDP Sciences; Astronomy and Astrophysics; 690; A78; 9-2024; 78-860004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202451161info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202451161info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:13:50Zoai:ri.conicet.gov.ar:11336/261355instacron: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:34982025-10-22 12:13:50.674CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
title Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
spellingShingle Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
Blanco, A. B.
ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERRMAL
STARS: WOLF RAYET
RADIO CONTINUUM:STARS
title_short Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
title_full Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
title_fullStr Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
title_full_unstemmed Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
title_sort Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations
dc.creator.none.fl_str_mv Blanco, A. B.
De Becker, M.
Saha, A.
Tej, A.
Benaglia, Paula
author Blanco, A. B.
author_facet Blanco, A. B.
De Becker, M.
Saha, A.
Tej, A.
Benaglia, Paula
author_role author
author2 De Becker, M.
Saha, A.
Tej, A.
Benaglia, Paula
author2_role author
author
author
author
dc.subject.none.fl_str_mv ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERRMAL
STARS: WOLF RAYET
RADIO CONTINUUM:STARS
topic ACCELERATION OF PARTICLES
RADIATION MECHANISMS: NON-THERRMAL
STARS: WOLF RAYET
RADIO CONTINUUM:STARS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. Massive stars produce strong stellar winds that consist of continuous outflows of material at speeds of thousands of km s‑1. These winds convey large amounts of kinetic power, especially in the case of Wolf–Rayet (WR) stars. When these winds interact with nearby material, they will likely produce shocks. Among other processes, particle acceleration is expected to occur. This is particularly well established in the case of massive binary systems, where the stellar winds collide, allowing these systems to be identified thanks to the detection of synchrotron radio emission, produced by a population of relativistic particles accelerated in the shocks. Aims. Our goal is to investigate the occurrence of particle acceleration among massive stars in their pre-supernova evolution phases. Methods. We observed a subset of five WR stars in the radio domain using the upgraded Giant Metrewave Radio Telescope (uGMRT), located in India. The observations were carried out in bands 4 (550–950 MHz) and 5 (1050–1450 MHz) for all the targets. Results. We detected radio emission for only WR 110 in bands 4 and 5. Its thermal spectrum displays a consistent index of +0.74 down to uGMRT bands. The four other targets were not detected and we derived 3σ upper limits on their flux density. Our upper limits in Band 4 are the first provided for these targets below 1 GHz. None of the targets was identified as a synchrotron radio emitter in these radio bands. Conclusions. If some synchrotron emission is produced in these systems, the non-detection with the uGMRT can be most likely attributed to strong free-free absorption (FFA). This is especially relevant for WR98a which is catalogued as a particle accelerator based on previous measurements at higher radio frequencies. The prominence of FFA constitutes a severe obstacle to identifying particle accelerators in the radio domain.
Fil: Blanco, A. B.. Université de Liège; Bélgica
Fil: De Becker, M.. Université de Liège; Bélgica
Fil: Saha, A.. Indian Institute Of Space Science And Technology; India
Fil: Tej, A.. Indian Institute Of Space Science And Technology; India
Fil: Benaglia, Paula. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
description Context. Massive stars produce strong stellar winds that consist of continuous outflows of material at speeds of thousands of km s‑1. These winds convey large amounts of kinetic power, especially in the case of Wolf–Rayet (WR) stars. When these winds interact with nearby material, they will likely produce shocks. Among other processes, particle acceleration is expected to occur. This is particularly well established in the case of massive binary systems, where the stellar winds collide, allowing these systems to be identified thanks to the detection of synchrotron radio emission, produced by a population of relativistic particles accelerated in the shocks. Aims. Our goal is to investigate the occurrence of particle acceleration among massive stars in their pre-supernova evolution phases. Methods. We observed a subset of five WR stars in the radio domain using the upgraded Giant Metrewave Radio Telescope (uGMRT), located in India. The observations were carried out in bands 4 (550–950 MHz) and 5 (1050–1450 MHz) for all the targets. Results. We detected radio emission for only WR 110 in bands 4 and 5. Its thermal spectrum displays a consistent index of +0.74 down to uGMRT bands. The four other targets were not detected and we derived 3σ upper limits on their flux density. Our upper limits in Band 4 are the first provided for these targets below 1 GHz. None of the targets was identified as a synchrotron radio emitter in these radio bands. Conclusions. If some synchrotron emission is produced in these systems, the non-detection with the uGMRT can be most likely attributed to strong free-free absorption (FFA). This is especially relevant for WR98a which is catalogued as a particle accelerator based on previous measurements at higher radio frequencies. The prominence of FFA constitutes a severe obstacle to identifying particle accelerators in the radio domain.
publishDate 2024
dc.date.none.fl_str_mv 2024-09
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/11336/261355
Blanco, A. B.; De Becker, M.; Saha, A.; Tej, A.; Benaglia, Paula; Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations; EDP Sciences; Astronomy and Astrophysics; 690; A78; 9-2024; 78-86
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/261355
identifier_str_mv Blanco, A. B.; De Becker, M.; Saha, A.; Tej, A.; Benaglia, Paula; Insight into the occurrence of particle acceleration through the investigation of Wolf–Rayet stars using uGMRT observations; EDP Sciences; Astronomy and Astrophysics; 690; A78; 9-2024; 78-86
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202451161
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202451161
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
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score 12.982451

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