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 CientiÂficas 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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/5008
Ver los metadatos del registro completo
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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 CientiÂficas 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 Técnicas2025-09-29T09:38:18Zoai: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:34982025-09-29 09:38:18.416CONICET 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 CientiÂficas 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 |
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CONICET Digital (CONICET) |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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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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13.070432 |