Discovering the colliding wind binary HD 93129A
- Autores
- Marcote, B.; Benaglia, Paula; Moldon, J.; Nelan, E.; De Becker, M.; Dougherty, S, M.; Koribalski, Bärbel
- Año de publicación
- 2015
- Idioma
- inglés
- Tipo de recurso
- documento de conferencia
- Estado
- versión publicada
- Descripción
- HD 93129A is a binary system including an O2 If+ and probably an O3.5 V-star orbiting at a distance of about 140 AU (55 mas given the distance of 2.5 kpc), which potentially makes the system the most massive one in the Galaxy, ahead of eta-Carina. Its non-thermal radio emission was proposed to be originated by the collision between the winds of both stars. HST/FGS data have been reanalyzed to derive an accurate absolute position of the stars to compare them with the radio emission. The analysis of ATCA radio observations along several years reveals a power-lawspectrum with an increase on the radio flux density along time. We conducted an observation with the Australian Long Baseline Array (LBA) at 2.3 GHz in 2008 to resolve the radio source and its location within the stellar system. These radio data revealed a bow-shape extended emissionlocated between both stars, as expected in a wind collision region. The observed structure allows us to roughly estimate the mass-loss rate ratio for the two stars in the system, concluding that dM_b/dt = 0.7 dM_a/dt. The multiwavelength analysis points out that the detected radio emission is likely to be originated by one of the most massive collision wind binary in the Galaxy.
Fil: Marcote, B.. Universidad de Barcelona; España
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
Fil: Moldon, J.. Netherlands Institute for Radio Astronomy; Países Bajos
Fil: Nelan, E.. Space Telescope Science Institute; Estados Unidos
Fil: De Becker, M.. Université de Liège; Bélgica
Fil: Dougherty, S, M.. NRC Herzberg Astronomy And Astrophysics; Canadá
Fil: Koribalski, Bärbel. Australia Telescope National Facility; Australia
12th European VLBI Network Symposium and Users Meeting
Cagliari
Italia
Istituto di Radioastronomia - Materia
-
RADIO CONTINUUM: STARS
STELLAR WINDS - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/139847
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Discovering the colliding wind binary HD 93129AMarcote, B.Benaglia, PaulaMoldon, J.Nelan, E.De Becker, M.Dougherty, S, M.Koribalski, BärbelRADIO CONTINUUM: STARSSTELLAR WINDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1HD 93129A is a binary system including an O2 If+ and probably an O3.5 V-star orbiting at a distance of about 140 AU (55 mas given the distance of 2.5 kpc), which potentially makes the system the most massive one in the Galaxy, ahead of eta-Carina. Its non-thermal radio emission was proposed to be originated by the collision between the winds of both stars. HST/FGS data have been reanalyzed to derive an accurate absolute position of the stars to compare them with the radio emission. The analysis of ATCA radio observations along several years reveals a power-lawspectrum with an increase on the radio flux density along time. We conducted an observation with the Australian Long Baseline Array (LBA) at 2.3 GHz in 2008 to resolve the radio source and its location within the stellar system. These radio data revealed a bow-shape extended emissionlocated between both stars, as expected in a wind collision region. The observed structure allows us to roughly estimate the mass-loss rate ratio for the two stars in the system, concluding that dM_b/dt = 0.7 dM_a/dt. The multiwavelength analysis points out that the detected radio emission is likely to be originated by one of the most massive collision wind binary in the Galaxy.Fil: Marcote, B.. Universidad de Barcelona; EspañaFil: 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; ArgentinaFil: Moldon, J.. Netherlands Institute for Radio Astronomy; Países BajosFil: Nelan, E.. Space Telescope Science Institute; Estados UnidosFil: De Becker, M.. Université de Liège; BélgicaFil: Dougherty, S, M.. NRC Herzberg Astronomy And Astrophysics; CanadáFil: Koribalski, Bärbel. Australia Telescope National Facility; Australia12th European VLBI Network Symposium and Users MeetingCagliariItaliaIstituto di RadioastronomiaSissaTarchi, AndreaGiroletti, MarcelloFeretti, Luigina2015info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/conferenceObjectSimposioBookhttp://purl.org/coar/resource_type/c_5794info:ar-repo/semantics/documentoDeConferenciaapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/139847Discovering the colliding wind binary HD 93129A; 12th European VLBI Network Symposium and Users Meeting; Cagliari; Italia; 2014; 1-51824-8039CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://pos.sissa.it/cgi-bin/reader/conf.cgi?confid=230Internacionalinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:24:02Zoai:ri.conicet.gov.ar:11336/139847instacron: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:34982025-10-15 15:24:03.11CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Discovering the colliding wind binary HD 93129A |
title |
Discovering the colliding wind binary HD 93129A |
spellingShingle |
Discovering the colliding wind binary HD 93129A Marcote, B. RADIO CONTINUUM: STARS STELLAR WINDS |
title_short |
Discovering the colliding wind binary HD 93129A |
title_full |
Discovering the colliding wind binary HD 93129A |
title_fullStr |
Discovering the colliding wind binary HD 93129A |
title_full_unstemmed |
Discovering the colliding wind binary HD 93129A |
title_sort |
Discovering the colliding wind binary HD 93129A |
dc.creator.none.fl_str_mv |
Marcote, B. Benaglia, Paula Moldon, J. Nelan, E. De Becker, M. Dougherty, S, M. Koribalski, Bärbel |
author |
Marcote, B. |
author_facet |
Marcote, B. Benaglia, Paula Moldon, J. Nelan, E. De Becker, M. Dougherty, S, M. Koribalski, Bärbel |
author_role |
author |
author2 |
Benaglia, Paula Moldon, J. Nelan, E. De Becker, M. Dougherty, S, M. Koribalski, Bärbel |
author2_role |
author author author author author author |
dc.contributor.none.fl_str_mv |
Tarchi, Andrea Giroletti, Marcello Feretti, Luigina |
dc.subject.none.fl_str_mv |
RADIO CONTINUUM: STARS STELLAR WINDS |
topic |
RADIO CONTINUUM: STARS STELLAR WINDS |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
HD 93129A is a binary system including an O2 If+ and probably an O3.5 V-star orbiting at a distance of about 140 AU (55 mas given the distance of 2.5 kpc), which potentially makes the system the most massive one in the Galaxy, ahead of eta-Carina. Its non-thermal radio emission was proposed to be originated by the collision between the winds of both stars. HST/FGS data have been reanalyzed to derive an accurate absolute position of the stars to compare them with the radio emission. The analysis of ATCA radio observations along several years reveals a power-lawspectrum with an increase on the radio flux density along time. We conducted an observation with the Australian Long Baseline Array (LBA) at 2.3 GHz in 2008 to resolve the radio source and its location within the stellar system. These radio data revealed a bow-shape extended emissionlocated between both stars, as expected in a wind collision region. The observed structure allows us to roughly estimate the mass-loss rate ratio for the two stars in the system, concluding that dM_b/dt = 0.7 dM_a/dt. The multiwavelength analysis points out that the detected radio emission is likely to be originated by one of the most massive collision wind binary in the Galaxy. Fil: Marcote, B.. Universidad de Barcelona; España 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 Fil: Moldon, J.. Netherlands Institute for Radio Astronomy; Países Bajos Fil: Nelan, E.. Space Telescope Science Institute; Estados Unidos Fil: De Becker, M.. Université de Liège; Bélgica Fil: Dougherty, S, M.. NRC Herzberg Astronomy And Astrophysics; Canadá Fil: Koribalski, Bärbel. Australia Telescope National Facility; Australia 12th European VLBI Network Symposium and Users Meeting Cagliari Italia Istituto di Radioastronomia |
description |
HD 93129A is a binary system including an O2 If+ and probably an O3.5 V-star orbiting at a distance of about 140 AU (55 mas given the distance of 2.5 kpc), which potentially makes the system the most massive one in the Galaxy, ahead of eta-Carina. Its non-thermal radio emission was proposed to be originated by the collision between the winds of both stars. HST/FGS data have been reanalyzed to derive an accurate absolute position of the stars to compare them with the radio emission. The analysis of ATCA radio observations along several years reveals a power-lawspectrum with an increase on the radio flux density along time. We conducted an observation with the Australian Long Baseline Array (LBA) at 2.3 GHz in 2008 to resolve the radio source and its location within the stellar system. These radio data revealed a bow-shape extended emissionlocated between both stars, as expected in a wind collision region. The observed structure allows us to roughly estimate the mass-loss rate ratio for the two stars in the system, concluding that dM_b/dt = 0.7 dM_a/dt. The multiwavelength analysis points out that the detected radio emission is likely to be originated by one of the most massive collision wind binary in the Galaxy. |
publishDate |
2015 |
dc.date.none.fl_str_mv |
2015 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/publishedVersion info:eu-repo/semantics/conferenceObject Simposio Book http://purl.org/coar/resource_type/c_5794 info:ar-repo/semantics/documentoDeConferencia |
status_str |
publishedVersion |
format |
conferenceObject |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/139847 Discovering the colliding wind binary HD 93129A; 12th European VLBI Network Symposium and Users Meeting; Cagliari; Italia; 2014; 1-5 1824-8039 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/139847 |
identifier_str_mv |
Discovering the colliding wind binary HD 93129A; 12th European VLBI Network Symposium and Users Meeting; Cagliari; Italia; 2014; 1-5 1824-8039 CONICET Digital CONICET |
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eng |
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eng |
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Internacional |
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Sissa |
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Sissa |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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