Characterizing Magnetic Properties of Young Protostars in Orion

Autores
Huang, Bo; Girart, Josep M.; Stephens, Ian W.; Myers, Philip C.; Zhang, Qizhou; Cortes, Paulo; Sánchez Monge, Álvaro; Fernandez Lopez, Manuel; Le Gouellec, Valentin J. M.; Megeath, Tom; Murillo, Nadia M.; Carpenter, John M.; Li, Zhi Yun; Liu, Junhao; Looney, Leslie W.; Sadavoy, Sarah; Karnath, Nicole; Kwon, Jungmi
Año de publicación
2025
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The B-field Orion Protostellar Survey (BOPS) recently obtained polarimetric observations at 870 μm toward 61 protostars in the Orion molecular clouds with ∼1″ spatial resolution using the Atacama Large Millimeter/submillimeter Array. From the BOPS sample, we selected the 26 protostars with extended polarized emission within a radius of ∼6″ (2400 au) around the protostar. This allows us to have sufficient statistical polarization data to infer the magnetic field strength. The magnetic field strength is derived using the Davis–Chandrasekhar–Fermi method. The underlying magnetic field strengths are approximately 2.0 mG for protostars with a standard hourglass magnetic field morphology, which is higher than the values derived for protostars with rotated hourglass, spiral, and complex magnetic field configurations (≲1.0 mG). This suggests that the magnetic field plays a more significant role in envelopes exhibiting a standard hourglass field morphology, and a value of ≳2.0 mG would be required to maintain such a structure at these scales. Furthermore, most protostars in the sample are slightly supercritical, with mass-to-flux ratios ≲3.0. In particular, the mass-to-flux ratios for all protostars with a standard hourglass magnetic field morphology are lower than 3.0. However, these ratios do not account for the contribution of the protostellar mass, which means they are likely significantly underestimated.
Fil: Huang, Bo. Consejo Superior de Investigaciones Científicas; España
Fil: Girart, Josep M.. Consejo Superior de Investigaciones Científicas; España
Fil: Stephens, Ian W.. Worcester State University; Estados Unidos
Fil: Myers, Philip C.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Cortes, Paulo. Joint Alma Observatory; Chile
Fil: Sánchez Monge, Álvaro. Consejo Superior de Investigaciones Científicas; España
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Le Gouellec, Valentin J. M.. Space Science And Astrobiology Division; Estados Unidos
Fil: Megeath, Tom. University Of Toledo (utoledo); Estados Unidos
Fil: Murillo, Nadia M.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Carpenter, John M.. National Radio Astronomy Observatory; Estados Unidos
Fil: Li, Zhi Yun. University of Virginia; Estados Unidos
Fil: Liu, Junhao. National Astronomical Observatory Of Japan; Japón
Fil: Looney, Leslie W.. University of Illinois. Urbana - Champaign; Estados Unidos
Fil: Sadavoy, Sarah. Queens University; Canadá
Fil: Karnath, Nicole. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Kwon, Jungmi. Korea Astronomy And Space Science Institute; Corea del Sur
Materia
Star formation
Interstellar 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:11336/279056
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/279056
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Characterizing Magnetic Properties of Young Protostars in OrionHuang, BoGirart, Josep M.Stephens, Ian W.Myers, Philip C.Zhang, QizhouCortes, PauloSánchez Monge, ÁlvaroFernandez Lopez, ManuelLe Gouellec, Valentin J. M.Megeath, TomMurillo, Nadia M.Carpenter, John M.Li, Zhi YunLiu, JunhaoLooney, Leslie W.Sadavoy, SarahKarnath, NicoleKwon, JungmiStar formationInterstellar magnetic fieldshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The B-field Orion Protostellar Survey (BOPS) recently obtained polarimetric observations at 870 μm toward 61 protostars in the Orion molecular clouds with ∼1″ spatial resolution using the Atacama Large Millimeter/submillimeter Array. From the BOPS sample, we selected the 26 protostars with extended polarized emission within a radius of ∼6″ (2400 au) around the protostar. This allows us to have sufficient statistical polarization data to infer the magnetic field strength. The magnetic field strength is derived using the Davis–Chandrasekhar–Fermi method. The underlying magnetic field strengths are approximately 2.0 mG for protostars with a standard hourglass magnetic field morphology, which is higher than the values derived for protostars with rotated hourglass, spiral, and complex magnetic field configurations (≲1.0 mG). This suggests that the magnetic field plays a more significant role in envelopes exhibiting a standard hourglass field morphology, and a value of ≳2.0 mG would be required to maintain such a structure at these scales. Furthermore, most protostars in the sample are slightly supercritical, with mass-to-flux ratios ≲3.0. In particular, the mass-to-flux ratios for all protostars with a standard hourglass magnetic field morphology are lower than 3.0. However, these ratios do not account for the contribution of the protostellar mass, which means they are likely significantly underestimated.Fil: Huang, Bo. Consejo Superior de Investigaciones Científicas; EspañaFil: Girart, Josep M.. Consejo Superior de Investigaciones Científicas; EspañaFil: Stephens, Ian W.. Worcester State University; Estados UnidosFil: Myers, Philip C.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Cortes, Paulo. Joint Alma Observatory; ChileFil: Sánchez Monge, Álvaro. Consejo Superior de Investigaciones Científicas; EspañaFil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Le Gouellec, Valentin J. M.. Space Science And Astrobiology Division; Estados UnidosFil: Megeath, Tom. University Of Toledo (utoledo); Estados UnidosFil: Murillo, Nadia M.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; MéxicoFil: Carpenter, John M.. National Radio Astronomy Observatory; Estados UnidosFil: Li, Zhi Yun. University of Virginia; Estados UnidosFil: Liu, Junhao. National Astronomical Observatory Of Japan; JapónFil: Looney, Leslie W.. University of Illinois. Urbana - Champaign; Estados UnidosFil: Sadavoy, Sarah. Queens University; CanadáFil: Karnath, Nicole. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Kwon, Jungmi. Korea Astronomy And Space Science Institute; Corea del SurIOP Publishing2025-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/279056Huang, Bo; Girart, Josep M.; Stephens, Ian W.; Myers, Philip C.; Zhang, Qizhou; et al.; Characterizing Magnetic Properties of Young Protostars in Orion; IOP Publishing; Astrophysical Journal; 984; 1; 4-2025; 1-100004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/adc30binfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/adc30binfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-02-26T10:06:36Zoai:ri.conicet.gov.ar:11336/279056instacron: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:34982026-02-26 10:06:36.675CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Characterizing Magnetic Properties of Young Protostars in Orion
title Characterizing Magnetic Properties of Young Protostars in Orion
spellingShingle Characterizing Magnetic Properties of Young Protostars in Orion
Huang, Bo
Star formation
Interstellar magnetic fields
title_short Characterizing Magnetic Properties of Young Protostars in Orion
title_full Characterizing Magnetic Properties of Young Protostars in Orion
title_fullStr Characterizing Magnetic Properties of Young Protostars in Orion
title_full_unstemmed Characterizing Magnetic Properties of Young Protostars in Orion
title_sort Characterizing Magnetic Properties of Young Protostars in Orion
dc.creator.none.fl_str_mv Huang, Bo
Girart, Josep M.
Stephens, Ian W.
Myers, Philip C.
Zhang, Qizhou
Cortes, Paulo
Sánchez Monge, Álvaro
Fernandez Lopez, Manuel
Le Gouellec, Valentin J. M.
Megeath, Tom
Murillo, Nadia M.
Carpenter, John M.
Li, Zhi Yun
Liu, Junhao
Looney, Leslie W.
Sadavoy, Sarah
Karnath, Nicole
Kwon, Jungmi
author Huang, Bo
author_facet Huang, Bo
Girart, Josep M.
Stephens, Ian W.
Myers, Philip C.
Zhang, Qizhou
Cortes, Paulo
Sánchez Monge, Álvaro
Fernandez Lopez, Manuel
Le Gouellec, Valentin J. M.
Megeath, Tom
Murillo, Nadia M.
Carpenter, John M.
Li, Zhi Yun
Liu, Junhao
Looney, Leslie W.
Sadavoy, Sarah
Karnath, Nicole
Kwon, Jungmi
author_role author
author2 Girart, Josep M.
Stephens, Ian W.
Myers, Philip C.
Zhang, Qizhou
Cortes, Paulo
Sánchez Monge, Álvaro
Fernandez Lopez, Manuel
Le Gouellec, Valentin J. M.
Megeath, Tom
Murillo, Nadia M.
Carpenter, John M.
Li, Zhi Yun
Liu, Junhao
Looney, Leslie W.
Sadavoy, Sarah
Karnath, Nicole
Kwon, Jungmi
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Star formation
Interstellar magnetic fields
topic Star formation
Interstellar 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 The B-field Orion Protostellar Survey (BOPS) recently obtained polarimetric observations at 870 μm toward 61 protostars in the Orion molecular clouds with ∼1″ spatial resolution using the Atacama Large Millimeter/submillimeter Array. From the BOPS sample, we selected the 26 protostars with extended polarized emission within a radius of ∼6″ (2400 au) around the protostar. This allows us to have sufficient statistical polarization data to infer the magnetic field strength. The magnetic field strength is derived using the Davis–Chandrasekhar–Fermi method. The underlying magnetic field strengths are approximately 2.0 mG for protostars with a standard hourglass magnetic field morphology, which is higher than the values derived for protostars with rotated hourglass, spiral, and complex magnetic field configurations (≲1.0 mG). This suggests that the magnetic field plays a more significant role in envelopes exhibiting a standard hourglass field morphology, and a value of ≳2.0 mG would be required to maintain such a structure at these scales. Furthermore, most protostars in the sample are slightly supercritical, with mass-to-flux ratios ≲3.0. In particular, the mass-to-flux ratios for all protostars with a standard hourglass magnetic field morphology are lower than 3.0. However, these ratios do not account for the contribution of the protostellar mass, which means they are likely significantly underestimated.
Fil: Huang, Bo. Consejo Superior de Investigaciones Científicas; España
Fil: Girart, Josep M.. Consejo Superior de Investigaciones Científicas; España
Fil: Stephens, Ian W.. Worcester State University; Estados Unidos
Fil: Myers, Philip C.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Cortes, Paulo. Joint Alma Observatory; Chile
Fil: Sánchez Monge, Álvaro. Consejo Superior de Investigaciones Científicas; España
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Le Gouellec, Valentin J. M.. Space Science And Astrobiology Division; Estados Unidos
Fil: Megeath, Tom. University Of Toledo (utoledo); Estados Unidos
Fil: Murillo, Nadia M.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Carpenter, John M.. National Radio Astronomy Observatory; Estados Unidos
Fil: Li, Zhi Yun. University of Virginia; Estados Unidos
Fil: Liu, Junhao. National Astronomical Observatory Of Japan; Japón
Fil: Looney, Leslie W.. University of Illinois. Urbana - Champaign; Estados Unidos
Fil: Sadavoy, Sarah. Queens University; Canadá
Fil: Karnath, Nicole. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Kwon, Jungmi. Korea Astronomy And Space Science Institute; Corea del Sur
description The B-field Orion Protostellar Survey (BOPS) recently obtained polarimetric observations at 870 μm toward 61 protostars in the Orion molecular clouds with ∼1″ spatial resolution using the Atacama Large Millimeter/submillimeter Array. From the BOPS sample, we selected the 26 protostars with extended polarized emission within a radius of ∼6″ (2400 au) around the protostar. This allows us to have sufficient statistical polarization data to infer the magnetic field strength. The magnetic field strength is derived using the Davis–Chandrasekhar–Fermi method. The underlying magnetic field strengths are approximately 2.0 mG for protostars with a standard hourglass magnetic field morphology, which is higher than the values derived for protostars with rotated hourglass, spiral, and complex magnetic field configurations (≲1.0 mG). This suggests that the magnetic field plays a more significant role in envelopes exhibiting a standard hourglass field morphology, and a value of ≳2.0 mG would be required to maintain such a structure at these scales. Furthermore, most protostars in the sample are slightly supercritical, with mass-to-flux ratios ≲3.0. In particular, the mass-to-flux ratios for all protostars with a standard hourglass magnetic field morphology are lower than 3.0. However, these ratios do not account for the contribution of the protostellar mass, which means they are likely significantly underestimated.
publishDate 2025
dc.date.none.fl_str_mv 2025-04
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/11336/279056
Huang, Bo; Girart, Josep M.; Stephens, Ian W.; Myers, Philip C.; Zhang, Qizhou; et al.; Characterizing Magnetic Properties of Young Protostars in Orion; IOP Publishing; Astrophysical Journal; 984; 1; 4-2025; 1-10
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/279056
identifier_str_mv Huang, Bo; Girart, Josep M.; Stephens, Ian W.; Myers, Philip C.; Zhang, Qizhou; et al.; Characterizing Magnetic Properties of Young Protostars in Orion; IOP Publishing; Astrophysical Journal; 984; 1; 4-2025; 1-10
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/adc30b
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/adc30b
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 13.176822

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