Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra

Autores
Wanderley, Fábio; Cunha, Katia; Kochukhov, Oleg; Smith, Verne V.; Souto, Diogo; Cao, Lyra; Covey, Kevin; Majewski, Steven R.; Martínez, Cintia Fernanda; Muirhead, Philip S.; Pinsonneault, Marc; Allende Prieto, C.; Stassun, Keivan G.
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Average magnetic field measurements are presented for 62 M-dwarf members of the Pleiades open cluster, derived from Zeeman-enhanced Fe I lines in the H band. A Markov Chain Monte Carlo methodology was employed to model magnetic filling factors using Sloan Digital Sky Survey (SDSS) IV APOGEE high-resolution spectra, along with the radiative transfer code Synmast, MARCS stellar atmosphere models, and the APOGEE Data Release 17 spectral line list. There is a positive correlation between mean magnetic fields and stellar rotation, with slow-rotator stars (Rossby number, Ro > 0.13) exhibiting a steeper slope than rapid rotators (Ro < 0.13). However, the lattersample still shows a positive trend between Ro and magnetic fields, which is given by 〈B〉 = 1604 × Ro−0.20. The derived stellar radii when compared with physical isochrones show that, on average, our sample shows radius inflation, with median enhanced radii ranging from +3.0% to +7.0%, depending on the model. There is a positive correlation between magnetic field strength and radius inflation, as well as with stellar spot coverage, correlations which together indicate that stellar spot-filling factors generated by strong magnetic fields might be the mechanism that drives radius inflation in these stars. We also compare our derived magnetic fields with chromospheric emission lines (Hα, Hβ, and Ca II K), as well as with X-ray and Hα to bolometric luminosity ratios, and find thatstars with higher chromospheric and coronal activity tend to be more magnetic.
Fil: Wanderley, Fábio. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Cunha, Katia. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Kochukhov, Oleg. Uppsala Universitet; Suecia
Fil: Smith, Verne V.. No especifíca;
Fil: Souto, Diogo. Universidade Federal de Sergipe; Brasil
Fil: Cao, Lyra. Ohio State University; Estados Unidos
Fil: Covey, Kevin. Western Washington University.; Estados Unidos
Fil: Majewski, Steven R.. University of Virginia; Estados Unidos
Fil: Martínez, Cintia Fernanda. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Fil: Muirhead, Philip S.. University Of Boston. Departament Astronomy; Estados Unidos
Fil: Pinsonneault, Marc. Ohio University; Estados Unidos
Fil: Allende Prieto, C.. Universidad de La Laguna; España
Fil: Stassun, Keivan G.. Vanderbilt University; Estados Unidos
Materia
NEAR INFRARED ASTRONOMY
OPEN STAR CLUSTERS
M DWARF STARS
STELLAR ACTIVITY
STELLAR MAGNETIC FIELDS
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:11336/275202
Acceder
id CONICETDig_6b4def9eb6f839d0f77901633e170b92
oai_identifier_str oai:ri.conicet.gov.ar:11336/275202
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE SpectraWanderley, FábioCunha, KatiaKochukhov, OlegSmith, Verne V.Souto, DiogoCao, LyraCovey, KevinMajewski, Steven R.Martínez, Cintia FernandaMuirhead, Philip S.Pinsonneault, MarcAllende Prieto, C.Stassun, Keivan G.NEAR INFRARED ASTRONOMYOPEN STAR CLUSTERSM DWARF STARSSTELLAR ACTIVITYSTELLAR MAGNETIC FIELDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Average magnetic field measurements are presented for 62 M-dwarf members of the Pleiades open cluster, derived from Zeeman-enhanced Fe I lines in the H band. A Markov Chain Monte Carlo methodology was employed to model magnetic filling factors using Sloan Digital Sky Survey (SDSS) IV APOGEE high-resolution spectra, along with the radiative transfer code Synmast, MARCS stellar atmosphere models, and the APOGEE Data Release 17 spectral line list. There is a positive correlation between mean magnetic fields and stellar rotation, with slow-rotator stars (Rossby number, Ro > 0.13) exhibiting a steeper slope than rapid rotators (Ro < 0.13). However, the lattersample still shows a positive trend between Ro and magnetic fields, which is given by 〈B〉 = 1604 × Ro−0.20. The derived stellar radii when compared with physical isochrones show that, on average, our sample shows radius inflation, with median enhanced radii ranging from +3.0% to +7.0%, depending on the model. There is a positive correlation between magnetic field strength and radius inflation, as well as with stellar spot coverage, correlations which together indicate that stellar spot-filling factors generated by strong magnetic fields might be the mechanism that drives radius inflation in these stars. We also compare our derived magnetic fields with chromospheric emission lines (Hα, Hβ, and Ca II K), as well as with X-ray and Hα to bolometric luminosity ratios, and find thatstars with higher chromospheric and coronal activity tend to be more magnetic.Fil: Wanderley, Fábio. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Cunha, Katia. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Kochukhov, Oleg. Uppsala Universitet; SueciaFil: Smith, Verne V.. No especifíca;Fil: Souto, Diogo. Universidade Federal de Sergipe; BrasilFil: Cao, Lyra. Ohio State University; Estados UnidosFil: Covey, Kevin. Western Washington University.; Estados UnidosFil: Majewski, Steven R.. University of Virginia; Estados UnidosFil: Martínez, Cintia Fernanda. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; ArgentinaFil: Muirhead, Philip S.. University Of Boston. Departament Astronomy; Estados UnidosFil: Pinsonneault, Marc. Ohio University; Estados UnidosFil: Allende Prieto, C.. Universidad de La Laguna; EspañaFil: Stassun, Keivan G.. Vanderbilt University; Estados UnidosIOP Publishing2024-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/275202Wanderley, Fábio; Cunha, Katia; Kochukhov, Oleg; Smith, Verne V.; Souto, Diogo; et al.; Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra; IOP Publishing; Astrophysical Journal; 971; 1; 8-2024; 1-130004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad571finfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad571finfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-12-03T08:39:42Zoai:ri.conicet.gov.ar:11336/275202instacron: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:34982025-12-03 08:39:43.138CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
title Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
spellingShingle Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
Wanderley, Fábio
NEAR INFRARED ASTRONOMY
OPEN STAR CLUSTERS
M DWARF STARS
STELLAR ACTIVITY
STELLAR MAGNETIC FIELDS
title_short Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
title_full Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
title_fullStr Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
title_full_unstemmed Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
title_sort Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra
dc.creator.none.fl_str_mv Wanderley, Fábio
Cunha, Katia
Kochukhov, Oleg
Smith, Verne V.
Souto, Diogo
Cao, Lyra
Covey, Kevin
Majewski, Steven R.
Martínez, Cintia Fernanda
Muirhead, Philip S.
Pinsonneault, Marc
Allende Prieto, C.
Stassun, Keivan G.
author Wanderley, Fábio
author_facet Wanderley, Fábio
Cunha, Katia
Kochukhov, Oleg
Smith, Verne V.
Souto, Diogo
Cao, Lyra
Covey, Kevin
Majewski, Steven R.
Martínez, Cintia Fernanda
Muirhead, Philip S.
Pinsonneault, Marc
Allende Prieto, C.
Stassun, Keivan G.
author_role author
author2 Cunha, Katia
Kochukhov, Oleg
Smith, Verne V.
Souto, Diogo
Cao, Lyra
Covey, Kevin
Majewski, Steven R.
Martínez, Cintia Fernanda
Muirhead, Philip S.
Pinsonneault, Marc
Allende Prieto, C.
Stassun, Keivan G.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv NEAR INFRARED ASTRONOMY
OPEN STAR CLUSTERS
M DWARF STARS
STELLAR ACTIVITY
STELLAR MAGNETIC FIELDS
topic NEAR INFRARED ASTRONOMY
OPEN STAR CLUSTERS
M DWARF STARS
STELLAR ACTIVITY
STELLAR MAGNETIC FIELDS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Average magnetic field measurements are presented for 62 M-dwarf members of the Pleiades open cluster, derived from Zeeman-enhanced Fe I lines in the H band. A Markov Chain Monte Carlo methodology was employed to model magnetic filling factors using Sloan Digital Sky Survey (SDSS) IV APOGEE high-resolution spectra, along with the radiative transfer code Synmast, MARCS stellar atmosphere models, and the APOGEE Data Release 17 spectral line list. There is a positive correlation between mean magnetic fields and stellar rotation, with slow-rotator stars (Rossby number, Ro > 0.13) exhibiting a steeper slope than rapid rotators (Ro < 0.13). However, the lattersample still shows a positive trend between Ro and magnetic fields, which is given by 〈B〉 = 1604 × Ro−0.20. The derived stellar radii when compared with physical isochrones show that, on average, our sample shows radius inflation, with median enhanced radii ranging from +3.0% to +7.0%, depending on the model. There is a positive correlation between magnetic field strength and radius inflation, as well as with stellar spot coverage, correlations which together indicate that stellar spot-filling factors generated by strong magnetic fields might be the mechanism that drives radius inflation in these stars. We also compare our derived magnetic fields with chromospheric emission lines (Hα, Hβ, and Ca II K), as well as with X-ray and Hα to bolometric luminosity ratios, and find thatstars with higher chromospheric and coronal activity tend to be more magnetic.
Fil: Wanderley, Fábio. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Cunha, Katia. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Kochukhov, Oleg. Uppsala Universitet; Suecia
Fil: Smith, Verne V.. No especifíca;
Fil: Souto, Diogo. Universidade Federal de Sergipe; Brasil
Fil: Cao, Lyra. Ohio State University; Estados Unidos
Fil: Covey, Kevin. Western Washington University.; Estados Unidos
Fil: Majewski, Steven R.. University of Virginia; Estados Unidos
Fil: Martínez, Cintia Fernanda. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Fil: Muirhead, Philip S.. University Of Boston. Departament Astronomy; Estados Unidos
Fil: Pinsonneault, Marc. Ohio University; Estados Unidos
Fil: Allende Prieto, C.. Universidad de La Laguna; España
Fil: Stassun, Keivan G.. Vanderbilt University; Estados Unidos
description Average magnetic field measurements are presented for 62 M-dwarf members of the Pleiades open cluster, derived from Zeeman-enhanced Fe I lines in the H band. A Markov Chain Monte Carlo methodology was employed to model magnetic filling factors using Sloan Digital Sky Survey (SDSS) IV APOGEE high-resolution spectra, along with the radiative transfer code Synmast, MARCS stellar atmosphere models, and the APOGEE Data Release 17 spectral line list. There is a positive correlation between mean magnetic fields and stellar rotation, with slow-rotator stars (Rossby number, Ro > 0.13) exhibiting a steeper slope than rapid rotators (Ro < 0.13). However, the lattersample still shows a positive trend between Ro and magnetic fields, which is given by 〈B〉 = 1604 × Ro−0.20. The derived stellar radii when compared with physical isochrones show that, on average, our sample shows radius inflation, with median enhanced radii ranging from +3.0% to +7.0%, depending on the model. There is a positive correlation between magnetic field strength and radius inflation, as well as with stellar spot coverage, correlations which together indicate that stellar spot-filling factors generated by strong magnetic fields might be the mechanism that drives radius inflation in these stars. We also compare our derived magnetic fields with chromospheric emission lines (Hα, Hβ, and Ca II K), as well as with X-ray and Hα to bolometric luminosity ratios, and find thatstars with higher chromospheric and coronal activity tend to be more magnetic.
publishDate 2024
dc.date.none.fl_str_mv 2024-08
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/11336/275202
Wanderley, Fábio; Cunha, Katia; Kochukhov, Oleg; Smith, Verne V.; Souto, Diogo; et al.; Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra; IOP Publishing; Astrophysical Journal; 971; 1; 8-2024; 1-13
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/275202
identifier_str_mv Wanderley, Fábio; Cunha, Katia; Kochukhov, Oleg; Smith, Verne V.; Souto, Diogo; et al.; Magnetic Fields in M-dwarf Members of the Pleiades Open Cluster Using APOGEE Spectra; IOP Publishing; Astrophysical Journal; 971; 1; 8-2024; 1-13
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad571f
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad571f
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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 13.214268

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