The high-energy emission from HD 93129A near periastron
- Autores
- del Palacio, Santiago; García, Federico; Altamirano, D.; Barba, Rodolfo Hector; Bosch Ramon, Valentí; Corcoran, Michael; De Becker, M.; Hamaguchi, K.; Maíz Apellániz, Jesús; Munar Adrover, P.; Paredes, Josep Maria; Romero, Gustavo Esteban; Sana, H.; Tavani, M.; ud-Doula, A.
- Año de publicación
- 2020
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ∼18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, fNT,e < 0.02. In addition, we set a lower limit for the magnetic field in the wind-collision region as BWCR > 0.3 G. We also argue a putative interpretation of the emission from which we estimate fNT,e ≍ 0.006 and BWCR ≍ 0.5 G. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries.
Fil: del Palacio, Santiago. 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
Fil: García, Federico. 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
Fil: Altamirano, D.. University of Southampton Highfield Campus; Reino Unido
Fil: Barba, Rodolfo Hector. Universidad de La Serena; Chile
Fil: Bosch Ramon, Valentí. Universidad de Barcelona; España
Fil: Corcoran, Michael. National Aeronautics and Space Administration; Estados Unidos
Fil: De Becker, M.. University of Liege; Bélgica
Fil: Hamaguchi, K.. National Aeronautics and Space Administration; Estados Unidos
Fil: Maíz Apellániz, Jesús. Consejo Superior de Investigaciones Cientificas. Centro de Astrobiologia.; España
Fil: Munar Adrover, P.. Universidad de Barcelona; España
Fil: Paredes, Josep Maria. Universidad de Barcelona; España
Fil: Romero, Gustavo Esteban. 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
Fil: Sana, H.. Instituut voor Sterrenkund; Bélgica
Fil: Tavani, M.. INAF-IAPS; Italia
Fil: ud-Doula, A.. Penn State Scranton. Department of Physics; Estados Unidos - Materia
-
Acceleration of particles
Radiation mechanisms
X rays
Non-thermal mechanisms - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/108638
Ver los metadatos del registro completo
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The high-energy emission from HD 93129A near periastrondel Palacio, SantiagoGarcía, FedericoAltamirano, D.Barba, Rodolfo HectorBosch Ramon, ValentíCorcoran, MichaelDe Becker, M.Hamaguchi, K.Maíz Apellániz, JesúsMunar Adrover, P.Paredes, Josep MariaRomero, Gustavo EstebanSana, H.Tavani, M.ud-Doula, A.Acceleration of particlesRadiation mechanismsX raysNon-thermal mechanismshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ∼18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, fNT,e < 0.02. In addition, we set a lower limit for the magnetic field in the wind-collision region as BWCR > 0.3 G. We also argue a putative interpretation of the emission from which we estimate fNT,e ≍ 0.006 and BWCR ≍ 0.5 G. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries.Fil: del Palacio, Santiago. 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; ArgentinaFil: García, Federico. 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; ArgentinaFil: Altamirano, D.. University of Southampton Highfield Campus; Reino UnidoFil: Barba, Rodolfo Hector. Universidad de La Serena; ChileFil: Bosch Ramon, Valentí. Universidad de Barcelona; EspañaFil: Corcoran, Michael. National Aeronautics and Space Administration; Estados UnidosFil: De Becker, M.. University of Liege; BélgicaFil: Hamaguchi, K.. National Aeronautics and Space Administration; Estados UnidosFil: Maíz Apellániz, Jesús. Consejo Superior de Investigaciones Cientificas. Centro de Astrobiologia.; EspañaFil: Munar Adrover, P.. Universidad de Barcelona; EspañaFil: Paredes, Josep Maria. Universidad de Barcelona; EspañaFil: Romero, Gustavo Esteban. 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; ArgentinaFil: Sana, H.. Instituut voor Sterrenkund; BélgicaFil: Tavani, M.. INAF-IAPS; ItaliaFil: ud-Doula, A.. Penn State Scranton. Department of Physics; Estados UnidosWiley Blackwell Publishing, Inc2020-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/108638del Palacio, Santiago; García, Federico; Altamirano, D.; Barba, Rodolfo Hector; Bosch Ramon, Valentí; et al.; The high-energy emission from HD 93129A near periastron; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 494; 4; 6-2020; 6043-60520035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/494/4/6043/5829871info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/staa1156info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2004.10032info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-10T13:13:24Zoai:ri.conicet.gov.ar:11336/108638instacron: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:34982025-09-10 13:13:24.383CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
The high-energy emission from HD 93129A near periastron |
| title |
The high-energy emission from HD 93129A near periastron |
| spellingShingle |
The high-energy emission from HD 93129A near periastron del Palacio, Santiago Acceleration of particles Radiation mechanisms X rays Non-thermal mechanisms |
| title_short |
The high-energy emission from HD 93129A near periastron |
| title_full |
The high-energy emission from HD 93129A near periastron |
| title_fullStr |
The high-energy emission from HD 93129A near periastron |
| title_full_unstemmed |
The high-energy emission from HD 93129A near periastron |
| title_sort |
The high-energy emission from HD 93129A near periastron |
| dc.creator.none.fl_str_mv |
del Palacio, Santiago García, Federico Altamirano, D. Barba, Rodolfo Hector Bosch Ramon, Valentí Corcoran, Michael De Becker, M. Hamaguchi, K. Maíz Apellániz, Jesús Munar Adrover, P. Paredes, Josep Maria Romero, Gustavo Esteban Sana, H. Tavani, M. ud-Doula, A. |
| author |
del Palacio, Santiago |
| author_facet |
del Palacio, Santiago García, Federico Altamirano, D. Barba, Rodolfo Hector Bosch Ramon, Valentí Corcoran, Michael De Becker, M. Hamaguchi, K. Maíz Apellániz, Jesús Munar Adrover, P. Paredes, Josep Maria Romero, Gustavo Esteban Sana, H. Tavani, M. ud-Doula, A. |
| author_role |
author |
| author2 |
García, Federico Altamirano, D. Barba, Rodolfo Hector Bosch Ramon, Valentí Corcoran, Michael De Becker, M. Hamaguchi, K. Maíz Apellániz, Jesús Munar Adrover, P. Paredes, Josep Maria Romero, Gustavo Esteban Sana, H. Tavani, M. ud-Doula, A. |
| author2_role |
author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
Acceleration of particles Radiation mechanisms X rays Non-thermal mechanisms |
| topic |
Acceleration of particles Radiation mechanisms X rays Non-thermal mechanisms |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ∼18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, fNT,e < 0.02. In addition, we set a lower limit for the magnetic field in the wind-collision region as BWCR > 0.3 G. We also argue a putative interpretation of the emission from which we estimate fNT,e ≍ 0.006 and BWCR ≍ 0.5 G. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries. Fil: del Palacio, Santiago. 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 Fil: García, Federico. 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 Fil: Altamirano, D.. University of Southampton Highfield Campus; Reino Unido Fil: Barba, Rodolfo Hector. Universidad de La Serena; Chile Fil: Bosch Ramon, Valentí. Universidad de Barcelona; España Fil: Corcoran, Michael. National Aeronautics and Space Administration; Estados Unidos Fil: De Becker, M.. University of Liege; Bélgica Fil: Hamaguchi, K.. National Aeronautics and Space Administration; Estados Unidos Fil: Maíz Apellániz, Jesús. Consejo Superior de Investigaciones Cientificas. Centro de Astrobiologia.; España Fil: Munar Adrover, P.. Universidad de Barcelona; España Fil: Paredes, Josep Maria. Universidad de Barcelona; España Fil: Romero, Gustavo Esteban. 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 Fil: Sana, H.. Instituut voor Sterrenkund; Bélgica Fil: Tavani, M.. INAF-IAPS; Italia Fil: ud-Doula, A.. Penn State Scranton. Department of Physics; Estados Unidos |
| description |
We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ∼18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, fNT,e < 0.02. In addition, we set a lower limit for the magnetic field in the wind-collision region as BWCR > 0.3 G. We also argue a putative interpretation of the emission from which we estimate fNT,e ≍ 0.006 and BWCR ≍ 0.5 G. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020-06 |
| 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/11336/108638 del Palacio, Santiago; García, Federico; Altamirano, D.; Barba, Rodolfo Hector; Bosch Ramon, Valentí; et al.; The high-energy emission from HD 93129A near periastron; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 494; 4; 6-2020; 6043-6052 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/108638 |
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del Palacio, Santiago; García, Federico; Altamirano, D.; Barba, Rodolfo Hector; Bosch Ramon, Valentí; et al.; The high-energy emission from HD 93129A near periastron; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 494; 4; 6-2020; 6043-6052 0035-8711 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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Wiley Blackwell Publishing, Inc |
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