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
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/139847

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spelling 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
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Book
http://purl.org/coar/resource_type/c_5794
info:ar-repo/semantics/documentoDeConferencia
status_str publishedVersion
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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
dc.language.none.fl_str_mv eng
language eng
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