HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations

Autores
Gonzalez, Jorge Federico; Briquet, M.; Przybilla, N.; Nieva, M.-F.; De Cat, P.; Saesen, S.; Hubrig, S.; Thoul, A.; Pápics, P.I.; Palaversa, L.; Naef, D.; Neveu-Van Malle, M.; Järvinen, S.; Pollard, K.R.; Kilmartin, P.; Mowlavi, N.; Butler, K.
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. HD 96446 is a magnetic B2p He-strong star that has been reported to be a β Cep pulsator. We present a detailed spectroscopic analysis of this object based on an intensive observational data set obtained in a multisite campaign with the spectrographs CORALIE, FEROS, and HARPS (La Silla); UVES (Paranal); HERCULES (Mt. John Observatory); and GIRAFFE (SAAO). Methods. Radial velocities were measured by cross-correlations and analysed to detect periodic variations. On the other hand, the mean spectrum was fit with spectral synthesis to derive atmospheric parameters and chemical abundances. Results. From the analysis of radial velocities, HD 96446 was found to be a spectroscopic binary with a period of 799 days. The stellar companion, which contributes only ∼5% of the total flux, is an A0-Type star. A frequency analysis of the radial velocities allowed us to detect two pulsational modes with periods 2.23 h and 2.66 h. The main mode is most probably a low-inclination, dipole mode (l, m) = (1, 0), and the second pulsation mode corresponds to (l, m) = (2, 2) or to a pole-on (l, m) = (3, 2) configuration. In addition to radial velocities, the main pulsation mode is evidenced through small variations in the spectral morphology (temperature variations) and the light flux. The rotation period of 23.4 d, was detected through the variation in line intensities. Chemical abundances are unevenly distributed over the stellar surface, with helium concentrated at the negative magnetic pole and most metals strengthened at lower latitudes. The mean chemical abundance of helium is strongly abnormal, reaching a value of 0.60 (number fraction).
Fil: Gonzalez, Jorge Federico. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Briquet, M.. Leibniz Institute For Astrophysics Potsdam; Alemania. Université de Liège; Bélgica
Fil: Przybilla, N.. Universidad de Innsbruck; Austria
Fil: Nieva, M.-F.. Universidad de Innsbruck; Austria
Fil: De Cat, P.. Royal Observatory Of Belgium; Bélgica
Fil: Saesen, S.. Universidad de Ginebra; Suiza
Fil: Hubrig, S.. Leibniz Institute For Astrophysics Potsdam; Alemania
Fil: Thoul, A.. Université de Liège; Bélgica
Fil: Pápics, P.I.. Instituut voor Sterrenkunde; Bélgica
Fil: Palaversa, L.. Institute Of Astronomy; Austria. Universidad de Ginebra; Suiza
Fil: Naef, D.. Universidad de Ginebra; Suiza
Fil: Neveu-Van Malle, M.. Universidad de Ginebra; Suiza
Fil: Järvinen, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Pollard, K.R.. University of Canterbury; Nueva Zelanda
Fil: Kilmartin, P.. University of Canterbury; Nueva Zelanda
Fil: Mowlavi, N.. Universidad de Ginebra; Suiza
Fil: Butler, K.. Ludwig Maximilians Universitat; Alemania
Materia
BINARIES: SPECTROSCOPIC
STARS: CHEMICALLY PECULIAR
STARS: EARLY-TYPE
STARS: INDIVIDUAL: HD 96446
STARS: MAGNETIC FIELD
STARS: OSCILLATIONS
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:11336/124776
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/124776
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsationsGonzalez, Jorge FedericoBriquet, M.Przybilla, N.Nieva, M.-F.De Cat, P.Saesen, S.Hubrig, S.Thoul, A.Pápics, P.I.Palaversa, L.Naef, D.Neveu-Van Malle, M.Järvinen, S.Pollard, K.R.Kilmartin, P.Mowlavi, N.Butler, K.BINARIES: SPECTROSCOPICSTARS: CHEMICALLY PECULIARSTARS: EARLY-TYPESTARS: INDIVIDUAL: HD 96446STARS: MAGNETIC FIELDSTARS: OSCILLATIONShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. HD 96446 is a magnetic B2p He-strong star that has been reported to be a β Cep pulsator. We present a detailed spectroscopic analysis of this object based on an intensive observational data set obtained in a multisite campaign with the spectrographs CORALIE, FEROS, and HARPS (La Silla); UVES (Paranal); HERCULES (Mt. John Observatory); and GIRAFFE (SAAO). Methods. Radial velocities were measured by cross-correlations and analysed to detect periodic variations. On the other hand, the mean spectrum was fit with spectral synthesis to derive atmospheric parameters and chemical abundances. Results. From the analysis of radial velocities, HD 96446 was found to be a spectroscopic binary with a period of 799 days. The stellar companion, which contributes only ∼5% of the total flux, is an A0-Type star. A frequency analysis of the radial velocities allowed us to detect two pulsational modes with periods 2.23 h and 2.66 h. The main mode is most probably a low-inclination, dipole mode (l, m) = (1, 0), and the second pulsation mode corresponds to (l, m) = (2, 2) or to a pole-on (l, m) = (3, 2) configuration. In addition to radial velocities, the main pulsation mode is evidenced through small variations in the spectral morphology (temperature variations) and the light flux. The rotation period of 23.4 d, was detected through the variation in line intensities. Chemical abundances are unevenly distributed over the stellar surface, with helium concentrated at the negative magnetic pole and most metals strengthened at lower latitudes. The mean chemical abundance of helium is strongly abnormal, reaching a value of 0.60 (number fraction).Fil: Gonzalez, Jorge Federico. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Briquet, M.. Leibniz Institute For Astrophysics Potsdam; Alemania. Université de Liège; BélgicaFil: Przybilla, N.. Universidad de Innsbruck; AustriaFil: Nieva, M.-F.. Universidad de Innsbruck; AustriaFil: De Cat, P.. Royal Observatory Of Belgium; BélgicaFil: Saesen, S.. Universidad de Ginebra; SuizaFil: Hubrig, S.. Leibniz Institute For Astrophysics Potsdam; AlemaniaFil: Thoul, A.. Université de Liège; BélgicaFil: Pápics, P.I.. Instituut voor Sterrenkunde; BélgicaFil: Palaversa, L.. Institute Of Astronomy; Austria. Universidad de Ginebra; SuizaFil: Naef, D.. Universidad de Ginebra; SuizaFil: Neveu-Van Malle, M.. Universidad de Ginebra; SuizaFil: Järvinen, S.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Pollard, K.R.. University of Canterbury; Nueva ZelandaFil: Kilmartin, P.. University of Canterbury; Nueva ZelandaFil: Mowlavi, N.. Universidad de Ginebra; SuizaFil: Butler, K.. Ludwig Maximilians Universitat; AlemaniaEDP Sciences2019-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/124776Gonzalez, Jorge Federico; Briquet, M.; Przybilla, N.; Nieva, M.-F.; De Cat, P.; et al.; HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations; EDP Sciences; Astronomy and Astrophysics; 626; 6-2019; 1-150004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201935177info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:37:16Zoai:ri.conicet.gov.ar:11336/124776instacron: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 10:37:16.462CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
title HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
spellingShingle HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
Gonzalez, Jorge Federico
BINARIES: SPECTROSCOPIC
STARS: CHEMICALLY PECULIAR
STARS: EARLY-TYPE
STARS: INDIVIDUAL: HD 96446
STARS: MAGNETIC FIELD
STARS: OSCILLATIONS
title_short HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
title_full HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
title_fullStr HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
title_full_unstemmed HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
title_sort HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations
dc.creator.none.fl_str_mv Gonzalez, Jorge Federico
Briquet, M.
Przybilla, N.
Nieva, M.-F.
De Cat, P.
Saesen, S.
Hubrig, S.
Thoul, A.
Pápics, P.I.
Palaversa, L.
Naef, D.
Neveu-Van Malle, M.
Järvinen, S.
Pollard, K.R.
Kilmartin, P.
Mowlavi, N.
Butler, K.
author Gonzalez, Jorge Federico
author_facet Gonzalez, Jorge Federico
Briquet, M.
Przybilla, N.
Nieva, M.-F.
De Cat, P.
Saesen, S.
Hubrig, S.
Thoul, A.
Pápics, P.I.
Palaversa, L.
Naef, D.
Neveu-Van Malle, M.
Järvinen, S.
Pollard, K.R.
Kilmartin, P.
Mowlavi, N.
Butler, K.
author_role author
author2 Briquet, M.
Przybilla, N.
Nieva, M.-F.
De Cat, P.
Saesen, S.
Hubrig, S.
Thoul, A.
Pápics, P.I.
Palaversa, L.
Naef, D.
Neveu-Van Malle, M.
Järvinen, S.
Pollard, K.R.
Kilmartin, P.
Mowlavi, N.
Butler, K.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv BINARIES: SPECTROSCOPIC
STARS: CHEMICALLY PECULIAR
STARS: EARLY-TYPE
STARS: INDIVIDUAL: HD 96446
STARS: MAGNETIC FIELD
STARS: OSCILLATIONS
topic BINARIES: SPECTROSCOPIC
STARS: CHEMICALLY PECULIAR
STARS: EARLY-TYPE
STARS: INDIVIDUAL: HD 96446
STARS: MAGNETIC FIELD
STARS: OSCILLATIONS
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. HD 96446 is a magnetic B2p He-strong star that has been reported to be a β Cep pulsator. We present a detailed spectroscopic analysis of this object based on an intensive observational data set obtained in a multisite campaign with the spectrographs CORALIE, FEROS, and HARPS (La Silla); UVES (Paranal); HERCULES (Mt. John Observatory); and GIRAFFE (SAAO). Methods. Radial velocities were measured by cross-correlations and analysed to detect periodic variations. On the other hand, the mean spectrum was fit with spectral synthesis to derive atmospheric parameters and chemical abundances. Results. From the analysis of radial velocities, HD 96446 was found to be a spectroscopic binary with a period of 799 days. The stellar companion, which contributes only ∼5% of the total flux, is an A0-Type star. A frequency analysis of the radial velocities allowed us to detect two pulsational modes with periods 2.23 h and 2.66 h. The main mode is most probably a low-inclination, dipole mode (l, m) = (1, 0), and the second pulsation mode corresponds to (l, m) = (2, 2) or to a pole-on (l, m) = (3, 2) configuration. In addition to radial velocities, the main pulsation mode is evidenced through small variations in the spectral morphology (temperature variations) and the light flux. The rotation period of 23.4 d, was detected through the variation in line intensities. Chemical abundances are unevenly distributed over the stellar surface, with helium concentrated at the negative magnetic pole and most metals strengthened at lower latitudes. The mean chemical abundance of helium is strongly abnormal, reaching a value of 0.60 (number fraction).
Fil: Gonzalez, Jorge Federico. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Briquet, M.. Leibniz Institute For Astrophysics Potsdam; Alemania. Université de Liège; Bélgica
Fil: Przybilla, N.. Universidad de Innsbruck; Austria
Fil: Nieva, M.-F.. Universidad de Innsbruck; Austria
Fil: De Cat, P.. Royal Observatory Of Belgium; Bélgica
Fil: Saesen, S.. Universidad de Ginebra; Suiza
Fil: Hubrig, S.. Leibniz Institute For Astrophysics Potsdam; Alemania
Fil: Thoul, A.. Université de Liège; Bélgica
Fil: Pápics, P.I.. Instituut voor Sterrenkunde; Bélgica
Fil: Palaversa, L.. Institute Of Astronomy; Austria. Universidad de Ginebra; Suiza
Fil: Naef, D.. Universidad de Ginebra; Suiza
Fil: Neveu-Van Malle, M.. Universidad de Ginebra; Suiza
Fil: Järvinen, S.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Pollard, K.R.. University of Canterbury; Nueva Zelanda
Fil: Kilmartin, P.. University of Canterbury; Nueva Zelanda
Fil: Mowlavi, N.. Universidad de Ginebra; Suiza
Fil: Butler, K.. Ludwig Maximilians Universitat; Alemania
description Aims. HD 96446 is a magnetic B2p He-strong star that has been reported to be a β Cep pulsator. We present a detailed spectroscopic analysis of this object based on an intensive observational data set obtained in a multisite campaign with the spectrographs CORALIE, FEROS, and HARPS (La Silla); UVES (Paranal); HERCULES (Mt. John Observatory); and GIRAFFE (SAAO). Methods. Radial velocities were measured by cross-correlations and analysed to detect periodic variations. On the other hand, the mean spectrum was fit with spectral synthesis to derive atmospheric parameters and chemical abundances. Results. From the analysis of radial velocities, HD 96446 was found to be a spectroscopic binary with a period of 799 days. The stellar companion, which contributes only ∼5% of the total flux, is an A0-Type star. A frequency analysis of the radial velocities allowed us to detect two pulsational modes with periods 2.23 h and 2.66 h. The main mode is most probably a low-inclination, dipole mode (l, m) = (1, 0), and the second pulsation mode corresponds to (l, m) = (2, 2) or to a pole-on (l, m) = (3, 2) configuration. In addition to radial velocities, the main pulsation mode is evidenced through small variations in the spectral morphology (temperature variations) and the light flux. The rotation period of 23.4 d, was detected through the variation in line intensities. Chemical abundances are unevenly distributed over the stellar surface, with helium concentrated at the negative magnetic pole and most metals strengthened at lower latitudes. The mean chemical abundance of helium is strongly abnormal, reaching a value of 0.60 (number fraction).
publishDate 2019
dc.date.none.fl_str_mv 2019-06
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/11336/124776
Gonzalez, Jorge Federico; Briquet, M.; Przybilla, N.; Nieva, M.-F.; De Cat, P.; et al.; HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations; EDP Sciences; Astronomy and Astrophysics; 626; 6-2019; 1-15
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/124776
identifier_str_mv Gonzalez, Jorge Federico; Briquet, M.; Przybilla, N.; Nieva, M.-F.; De Cat, P.; et al.; HD 96446: A long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations; EDP Sciences; Astronomy and Astrophysics; 626; 6-2019; 1-15
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201935177
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
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 13.070432

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