B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions

Autores
Hubrig, S.; Fossati, L.; Carroll, T. A.; Castro, N.; Gonzalez, Jorge Federico; Ilyin, I.; Przybilla, N.; Schöller, M.; Oskinova, L. M.; Morel, T.; Langer, N.; Scholz, R. D.; Khachenko, N. V.; Nieva, M. F.; BOB collaboration
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. Recent magnetic field surveys in O- and B-type stars revealed that about 10% of the core-hydrogen-burning massive stars host large-scale magnetic fields. The physical origin of these fields is highly debated. To identify and model the physical processes responsible for the generation of magnetic fields in massive stars, it is important to establish whether magnetic massive stars are found in very young star-forming regions or whether they are formed in close interacting binary systems. Methods. In the framework of our ESO Large Program, we carried out low-resolution spectropolarimetric observations with FORS 2 in 2013 April of the three most massive central stars in the Trifid nebula, HD 164492A, HD 164492C, and HD 164492D. These observations indicated a strong longitudinal magnetic field of about 500–600 G in the poorly studied component HD 164492C. To confirm this detection, we used HARPS in spectropolarimetric mode on two consecutive nights in 2013 June. Results. Our HARPS observations confirmed the longitudinal magnetic field in HD 164492C. Furthermore, the HARPS observations revealed that HD 164492C cannot be considered as a single star as it possesses one or two companions. The spectral appearance indicates that the primary is most likely of spectral type B1–B1.5 V. Since in both observing nights most spectral lines appear blended, it is currently unclear which components are magnetic. Long-term monitoring using high-resolution spectropolarimetry is necessary to separate the contribution of each component to the magnetic signal. Given the location of the system HD 164492C in one of the youngest star formation regions, this system can be considered as a Rosetta Stone for our understanding of the origin of magnetic fields in massive stars.
Fil: Hubrig, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Fossati, L.. Universität Bonn. Argelander-Institut für Astronomie; Alemania
Fil: Carroll, T. A.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Castro, N.. Universität Bonn. Argelander-Institut für Astronomie; Alemania
Fil: Gonzalez, Jorge Federico. Consejo Nacional de Investigaciones Cienti­ficas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; Argentina
Fil: Ilyin, I.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Przybilla, N.. University of Innsbruck. Institute for Astro- and Particle Physics; Austria
Fil: Schöller, M. . European Southern Observatory; Alemania
Fil: Oskinova, L. M. . Universität Potsdam. Institut für Physik und Astronomie; Alemania
Fil: Morel, T. . Université de Liège. Institut d’Astrophysique et de Géophysique; Bélgica
Fil: Langer, N. . Universität Bonn. Argelander-Institut für Astronomie; Alemania
Fil: Scholz, R. D. . Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Khachenko, N. V.. Main Astronomical Observatory; Ucrania
Fil: Nieva, M. F.. Institute for Astro- and Particle Physics, University of Innsbruck; Austria. University Erlangen-Nuremberg. Dr. Karl Remeis-Observatory & ECAP; Alemania
Fil: BOB collaboration.
Materia
binaries: close, stars: early-type
stars: fundamental parameters
stars: magnetic field
stars: variables: general
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:11336/4985
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/4985
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regionsHubrig, S. Fossati, L.Carroll, T. A.Castro, N.Gonzalez, Jorge FedericoIlyin, I.Przybilla, N.Schöller, M. Oskinova, L. M. Morel, T. Langer, N. Scholz, R. D. Khachenko, N. V.Nieva, M. F.BOB collaborationbinaries: close, stars: early-typestars: fundamental parametersstars: magnetic fieldstars: variables: generalhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. Recent magnetic field surveys in O- and B-type stars revealed that about 10% of the core-hydrogen-burning massive stars host large-scale magnetic fields. The physical origin of these fields is highly debated. To identify and model the physical processes responsible for the generation of magnetic fields in massive stars, it is important to establish whether magnetic massive stars are found in very young star-forming regions or whether they are formed in close interacting binary systems. Methods. In the framework of our ESO Large Program, we carried out low-resolution spectropolarimetric observations with FORS 2 in 2013 April of the three most massive central stars in the Trifid nebula, HD 164492A, HD 164492C, and HD 164492D. These observations indicated a strong longitudinal magnetic field of about 500–600 G in the poorly studied component HD 164492C. To confirm this detection, we used HARPS in spectropolarimetric mode on two consecutive nights in 2013 June. Results. Our HARPS observations confirmed the longitudinal magnetic field in HD 164492C. Furthermore, the HARPS observations revealed that HD 164492C cannot be considered as a single star as it possesses one or two companions. The spectral appearance indicates that the primary is most likely of spectral type B1–B1.5 V. Since in both observing nights most spectral lines appear blended, it is currently unclear which components are magnetic. Long-term monitoring using high-resolution spectropolarimetry is necessary to separate the contribution of each component to the magnetic signal. Given the location of the system HD 164492C in one of the youngest star formation regions, this system can be considered as a Rosetta Stone for our understanding of the origin of magnetic fields in massive stars.Fil: Hubrig, S.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Fossati, L.. Universität Bonn. Argelander-Institut für Astronomie; AlemaniaFil: Carroll, T. A.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Castro, N.. Universität Bonn. Argelander-Institut für Astronomie; AlemaniaFil: Gonzalez, Jorge Federico. Consejo Nacional de Investigaciones Cienti­ficas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; ArgentinaFil: Ilyin, I.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Przybilla, N.. University of Innsbruck. Institute for Astro- and Particle Physics; AustriaFil: Schöller, M. . European Southern Observatory; AlemaniaFil: Oskinova, L. M. . Universität Potsdam. Institut für Physik und Astronomie; AlemaniaFil: Morel, T. . Université de Liège. Institut d’Astrophysique et de Géophysique; BélgicaFil: Langer, N. . Universität Bonn. Argelander-Institut für Astronomie; AlemaniaFil: Scholz, R. D. . Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Khachenko, N. V.. Main Astronomical Observatory; UcraniaFil: Nieva, M. F.. Institute for Astro- and Particle Physics, University of Innsbruck; Austria. University Erlangen-Nuremberg. Dr. Karl Remeis-Observatory & ECAP; AlemaniaFil: BOB collaboration.EDP Sciences2014-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/4985Hubrig, S.; Fossati, L.; Carroll, T. A.; Castro, N.; Gonzalez, Jorge Federico; et al.; B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions; EDP Sciences; Astronomy and Astrophysics; 564; L10; 4-2014; 1-50004-6361enginfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2014/04/aa23490-14/aa23490-14.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201423490info:eu-repo/semantics/altIdentifier/doi/info:eu-repo/semantics/altIdentifier/url/http://arxiv.org/abs/1403.0491info:eu-repo/semantics/altIdentifier/arxiv/1403.0491info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:36:34Zoai:ri.conicet.gov.ar:11336/4985instacron: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 15:36:35.24CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
title B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
spellingShingle B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
Hubrig, S.
binaries: close, stars: early-type
stars: fundamental parameters
stars: magnetic field
stars: variables: general
title_short B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
title_full B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
title_fullStr B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
title_full_unstemmed B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
title_sort B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions
dc.creator.none.fl_str_mv Hubrig, S.
Fossati, L.
Carroll, T. A.
Castro, N.
Gonzalez, Jorge Federico
Ilyin, I.
Przybilla, N.
Schöller, M.
Oskinova, L. M.
Morel, T.
Langer, N.
Scholz, R. D.
Khachenko, N. V.
Nieva, M. F.
BOB collaboration
author Hubrig, S.
author_facet Hubrig, S.
Fossati, L.
Carroll, T. A.
Castro, N.
Gonzalez, Jorge Federico
Ilyin, I.
Przybilla, N.
Schöller, M.
Oskinova, L. M.
Morel, T.
Langer, N.
Scholz, R. D.
Khachenko, N. V.
Nieva, M. F.
BOB collaboration
author_role author
author2 Fossati, L.
Carroll, T. A.
Castro, N.
Gonzalez, Jorge Federico
Ilyin, I.
Przybilla, N.
Schöller, M.
Oskinova, L. M.
Morel, T.
Langer, N.
Scholz, R. D.
Khachenko, N. V.
Nieva, M. F.
BOB collaboration
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv binaries: close, stars: early-type
stars: fundamental parameters
stars: magnetic field
stars: variables: general
topic binaries: close, stars: early-type
stars: fundamental parameters
stars: magnetic field
stars: variables: general
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. Recent magnetic field surveys in O- and B-type stars revealed that about 10% of the core-hydrogen-burning massive stars host large-scale magnetic fields. The physical origin of these fields is highly debated. To identify and model the physical processes responsible for the generation of magnetic fields in massive stars, it is important to establish whether magnetic massive stars are found in very young star-forming regions or whether they are formed in close interacting binary systems. Methods. In the framework of our ESO Large Program, we carried out low-resolution spectropolarimetric observations with FORS 2 in 2013 April of the three most massive central stars in the Trifid nebula, HD 164492A, HD 164492C, and HD 164492D. These observations indicated a strong longitudinal magnetic field of about 500–600 G in the poorly studied component HD 164492C. To confirm this detection, we used HARPS in spectropolarimetric mode on two consecutive nights in 2013 June. Results. Our HARPS observations confirmed the longitudinal magnetic field in HD 164492C. Furthermore, the HARPS observations revealed that HD 164492C cannot be considered as a single star as it possesses one or two companions. The spectral appearance indicates that the primary is most likely of spectral type B1–B1.5 V. Since in both observing nights most spectral lines appear blended, it is currently unclear which components are magnetic. Long-term monitoring using high-resolution spectropolarimetry is necessary to separate the contribution of each component to the magnetic signal. Given the location of the system HD 164492C in one of the youngest star formation regions, this system can be considered as a Rosetta Stone for our understanding of the origin of magnetic fields in massive stars.
Fil: Hubrig, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Fossati, L.. Universität Bonn. Argelander-Institut für Astronomie; Alemania
Fil: Carroll, T. A.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Castro, N.. Universität Bonn. Argelander-Institut für Astronomie; Alemania
Fil: Gonzalez, Jorge Federico. Consejo Nacional de Investigaciones Cienti­ficas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; Argentina
Fil: Ilyin, I.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Przybilla, N.. University of Innsbruck. Institute for Astro- and Particle Physics; Austria
Fil: Schöller, M. . European Southern Observatory; Alemania
Fil: Oskinova, L. M. . Universität Potsdam. Institut für Physik und Astronomie; Alemania
Fil: Morel, T. . Université de Liège. Institut d’Astrophysique et de Géophysique; Bélgica
Fil: Langer, N. . Universität Bonn. Argelander-Institut für Astronomie; Alemania
Fil: Scholz, R. D. . Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Khachenko, N. V.. Main Astronomical Observatory; Ucrania
Fil: Nieva, M. F.. Institute for Astro- and Particle Physics, University of Innsbruck; Austria. University Erlangen-Nuremberg. Dr. Karl Remeis-Observatory & ECAP; Alemania
Fil: BOB collaboration.
description Aims. Recent magnetic field surveys in O- and B-type stars revealed that about 10% of the core-hydrogen-burning massive stars host large-scale magnetic fields. The physical origin of these fields is highly debated. To identify and model the physical processes responsible for the generation of magnetic fields in massive stars, it is important to establish whether magnetic massive stars are found in very young star-forming regions or whether they are formed in close interacting binary systems. Methods. In the framework of our ESO Large Program, we carried out low-resolution spectropolarimetric observations with FORS 2 in 2013 April of the three most massive central stars in the Trifid nebula, HD 164492A, HD 164492C, and HD 164492D. These observations indicated a strong longitudinal magnetic field of about 500–600 G in the poorly studied component HD 164492C. To confirm this detection, we used HARPS in spectropolarimetric mode on two consecutive nights in 2013 June. Results. Our HARPS observations confirmed the longitudinal magnetic field in HD 164492C. Furthermore, the HARPS observations revealed that HD 164492C cannot be considered as a single star as it possesses one or two companions. The spectral appearance indicates that the primary is most likely of spectral type B1–B1.5 V. Since in both observing nights most spectral lines appear blended, it is currently unclear which components are magnetic. Long-term monitoring using high-resolution spectropolarimetry is necessary to separate the contribution of each component to the magnetic signal. Given the location of the system HD 164492C in one of the youngest star formation regions, this system can be considered as a Rosetta Stone for our understanding of the origin of magnetic fields in massive stars.
publishDate 2014
dc.date.none.fl_str_mv 2014-04
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/11336/4985
Hubrig, S.; Fossati, L.; Carroll, T. A.; Castro, N.; Gonzalez, Jorge Federico; et al.; B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions; EDP Sciences; Astronomy and Astrophysics; 564; L10; 4-2014; 1-5
0004-6361
url http://hdl.handle.net/11336/4985
identifier_str_mv Hubrig, S.; Fossati, L.; Carroll, T. A.; Castro, N.; Gonzalez, Jorge Federico; et al.; B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions; EDP Sciences; Astronomy and Astrophysics; 564; L10; 4-2014; 1-5
0004-6361
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2014/04/aa23490-14/aa23490-14.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201423490
info:eu-repo/semantics/altIdentifier/doi/
info:eu-repo/semantics/altIdentifier/url/http://arxiv.org/abs/1403.0491
info:eu-repo/semantics/altIdentifier/arxiv/1403.0491
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/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 13.22299

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