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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/261355
Ver los metadatos del registro completo
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CONICET Digital (CONICET) |
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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 Técnicas2025-09-29T10:41:17Zoai: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:34982025-09-29 10:41:17.497CONICET 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 |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.070432 |