HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation

Autores
Schöller, M.; Hubrig, S.; Correia, S.; Ilyin, I.; Gonzalez, Jorge Federico
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The most distinctive feature of HgMn stars is the extreme overabundance of heavy elements in their atmospheres. Furthermore, they show chemical horizontal and vertical inhomogeneities and kG mean quadratic magnetic fields. The topology of these magnetic fields should be rather complex, as we measure only weak mean longitudinal magnetic fields. The connection between these features and their membership in binary and multiple systems is supported by our observations during the last decade. The most important result achieved in our studies of a large sample of late B-type primaries in spectroscopic binaries and visual multiples is the finding that the vast majority of slowly rotating late B-type stars formed in binary systems with v sin i < 70 km s^{-1} and orbital periods between 3 and 20 days become HgMn stars.
Fil: Schöller, M.. European Southern Observatory; Alemania
Fil: Hubrig, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Correia, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Ilyin, I.. Leibniz-Institut für Astrophysik Potsdam; 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
Materia
Chemically Peculiar Stars
Hg-Mn Stars
Binaries
Magnetic Fields
Starspots
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:11336/5008
Acceder
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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star FormationSchöller, M.Hubrig, S.Correia, S.Ilyin, I.Gonzalez, Jorge FedericoChemically Peculiar StarsHg-Mn StarsBinariesMagnetic FieldsStarspotshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The most distinctive feature of HgMn stars is the extreme overabundance of heavy elements in their atmospheres. Furthermore, they show chemical horizontal and vertical inhomogeneities and kG mean quadratic magnetic fields. The topology of these magnetic fields should be rather complex, as we measure only weak mean longitudinal magnetic fields. The connection between these features and their membership in binary and multiple systems is supported by our observations during the last decade. The most important result achieved in our studies of a large sample of late B-type primaries in spectroscopic binaries and visual multiples is the finding that the vast majority of slowly rotating late B-type stars formed in binary systems with v sin i < 70 km s^{-1} and orbital periods between 3 and 20 days become HgMn stars.Fil: Schöller, M.. European Southern Observatory; AlemaniaFil: Hubrig, S.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Correia, S.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Ilyin, I.. Leibniz-Institut für Astrophysik Potsdam; 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; ArgentinaUniversity of Zagreb2013-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/5008Schöller, M.; Hubrig, S.; Correia, S.; Ilyin, I.; Gonzalez, Jorge Federico; HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation; University of Zagreb; Central European Astrophysical Bulletin; 37; 1-2013; 369-3791845-8319enginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2013CEAB...37..369Sinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:06:33Zoai:ri.conicet.gov.ar:11336/5008instacron: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:34982025-10-22 11:06:33.521CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
title HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
spellingShingle HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
Schöller, M.
Chemically Peculiar Stars
Hg-Mn Stars
Binaries
Magnetic Fields
Starspots
title_short HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
title_full HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
title_fullStr HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
title_full_unstemmed HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
title_sort HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation
dc.creator.none.fl_str_mv Schöller, M.
Hubrig, S.
Correia, S.
Ilyin, I.
Gonzalez, Jorge Federico
author Schöller, M.
author_facet Schöller, M.
Hubrig, S.
Correia, S.
Ilyin, I.
Gonzalez, Jorge Federico
author_role author
author2 Hubrig, S.
Correia, S.
Ilyin, I.
Gonzalez, Jorge Federico
author2_role author
author
author
author
dc.subject.none.fl_str_mv Chemically Peculiar Stars
Hg-Mn Stars
Binaries
Magnetic Fields
Starspots
topic Chemically Peculiar Stars
Hg-Mn Stars
Binaries
Magnetic Fields
Starspots
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The most distinctive feature of HgMn stars is the extreme overabundance of heavy elements in their atmospheres. Furthermore, they show chemical horizontal and vertical inhomogeneities and kG mean quadratic magnetic fields. The topology of these magnetic fields should be rather complex, as we measure only weak mean longitudinal magnetic fields. The connection between these features and their membership in binary and multiple systems is supported by our observations during the last decade. The most important result achieved in our studies of a large sample of late B-type primaries in spectroscopic binaries and visual multiples is the finding that the vast majority of slowly rotating late B-type stars formed in binary systems with v sin i < 70 km s^{-1} and orbital periods between 3 and 20 days become HgMn stars.
Fil: Schöller, M.. European Southern Observatory; Alemania
Fil: Hubrig, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Correia, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Ilyin, I.. Leibniz-Institut für Astrophysik Potsdam; 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
description The most distinctive feature of HgMn stars is the extreme overabundance of heavy elements in their atmospheres. Furthermore, they show chemical horizontal and vertical inhomogeneities and kG mean quadratic magnetic fields. The topology of these magnetic fields should be rather complex, as we measure only weak mean longitudinal magnetic fields. The connection between these features and their membership in binary and multiple systems is supported by our observations during the last decade. The most important result achieved in our studies of a large sample of late B-type primaries in spectroscopic binaries and visual multiples is the finding that the vast majority of slowly rotating late B-type stars formed in binary systems with v sin i < 70 km s^{-1} and orbital periods between 3 and 20 days become HgMn stars.
publishDate 2013
dc.date.none.fl_str_mv 2013-01
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/11336/5008
Schöller, M.; Hubrig, S.; Correia, S.; Ilyin, I.; Gonzalez, Jorge Federico; HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation; University of Zagreb; Central European Astrophysical Bulletin; 37; 1-2013; 369-379
1845-8319
url http://hdl.handle.net/11336/5008
identifier_str_mv Schöller, M.; Hubrig, S.; Correia, S.; Ilyin, I.; Gonzalez, Jorge Federico; HgMn Stars: Cornerstones for our Understanding of Late B-type Multiple Star Formation; University of Zagreb; Central European Astrophysical Bulletin; 37; 1-2013; 369-379
1845-8319
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2013CEAB...37..369S
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 University of Zagreb
publisher.none.fl_str_mv University of Zagreb
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 12.982451

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