Spatially resolved magnetic field structure in the disk of a T Tauri star
- Autores
- Stephens, Ian W.; Looney, Leslie W.; Kwon, Woojin; Fernandez Lopez, Manuel; Hughes, A. Meredith; Mundy, Lee G.; Crutcher, Richard M.; Li, Zhi Yun; Rao, Ramprasad
- Año de publicación
- 2014
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Magnetic fields in accretion disks play a dominant role during the star formation process but have hitherto been observationally poorly constrained. Field strengths have been inferred on T Tauri stars themselves and possibly in the innermost part of the accretion disk, but the strength and morphology of the field in the bulk of the disk have not been observed. Unresolved measurements of polarized emission (arising from elongated dust grains aligned perpendicular to the field) imply average fields aligned with the disks. Theoretically, the fields are expected to be largely toroidal, poloidal, or a mixture of the two, which imply different mechanisms for transporting angular momentum in the disks of actively accreting young stars such as HL Tau. Here we report resolved measurements of the polarized 1.25 mm continuum emission from HL Tau's disk. The magnetic field on a scale of 80 AU is coincident with the major axis (~210 AU diameter) of the disk. From this we conclude that the magnetic field inside the disk at this scale cannot be dominated by a vertical component, though a purely toroidal field does not fit the data well either. The unexpected morphology suggests that the magnetic field's role for the accretion of a T Tauri star is more complex than the current theoretical understanding.
Fil: Stephens, Ian W. . Boston University, Institute for Astrophysical Research; Estados Unidos
Fil: Looney, Leslie W. . University of Illinois, Urbana. Department of Astronomy; Estados Unidos
Fil: Kwon, Woojin . Netherlands Institute for Space Research, Groningen; Países Bajos
Fil: Fernandez Lopez, Manuel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); Argentina
Fil: Hughes, A. Meredith . Wesleyan University. Van Vleck Observatory, Astronomy Department ; Estados Unidos
Fil: Mundy, Lee G. . University of Maryland. Astronomy Department & Laboratory for Millimeter-wave Astronomy; Estados Unidos
Fil: Crutcher, Richard M. . University of Illinois, Urbana. Department of Astronomy; Estados Unidos
Fil: Li, Zhi Yun. University of Virginia. Astronomy Department; Estados Unidos
Fil: Rao, Ramprasad . Academia Sinica. Institute of Astronomy and Astrophysics; Estados Unidos - Materia
-
Star formation
Protostellar disks
Polarization
margnetic fields
T Tauri stars - 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:11336/7230
Ver los metadatos del registro completo
id |
CONICETDig_30bb9f3ad83ebe79669609620b7253d8 |
---|---|
oai_identifier_str |
oai:ri.conicet.gov.ar:11336/7230 |
network_acronym_str |
CONICETDig |
repository_id_str |
3498 |
network_name_str |
CONICET Digital (CONICET) |
spelling |
Spatially resolved magnetic field structure in the disk of a T Tauri starStephens, Ian W. Looney, Leslie W. Kwon, Woojin Fernandez Lopez, ManuelHughes, A. Meredith Mundy, Lee G. Crutcher, Richard M. Li, Zhi YunRao, Ramprasad Star formationProtostellar disksPolarizationmargnetic fieldsT Tauri starshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Magnetic fields in accretion disks play a dominant role during the star formation process but have hitherto been observationally poorly constrained. Field strengths have been inferred on T Tauri stars themselves and possibly in the innermost part of the accretion disk, but the strength and morphology of the field in the bulk of the disk have not been observed. Unresolved measurements of polarized emission (arising from elongated dust grains aligned perpendicular to the field) imply average fields aligned with the disks. Theoretically, the fields are expected to be largely toroidal, poloidal, or a mixture of the two, which imply different mechanisms for transporting angular momentum in the disks of actively accreting young stars such as HL Tau. Here we report resolved measurements of the polarized 1.25 mm continuum emission from HL Tau's disk. The magnetic field on a scale of 80 AU is coincident with the major axis (~210 AU diameter) of the disk. From this we conclude that the magnetic field inside the disk at this scale cannot be dominated by a vertical component, though a purely toroidal field does not fit the data well either. The unexpected morphology suggests that the magnetic field's role for the accretion of a T Tauri star is more complex than the current theoretical understanding.Fil: Stephens, Ian W. . Boston University, Institute for Astrophysical Research; Estados UnidosFil: Looney, Leslie W. . University of Illinois, Urbana. Department of Astronomy; Estados UnidosFil: Kwon, Woojin . Netherlands Institute for Space Research, Groningen; Países BajosFil: Fernandez Lopez, Manuel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); ArgentinaFil: Hughes, A. Meredith . Wesleyan University. Van Vleck Observatory, Astronomy Department ; Estados UnidosFil: Mundy, Lee G. . University of Maryland. Astronomy Department & Laboratory for Millimeter-wave Astronomy; Estados UnidosFil: Crutcher, Richard M. . University of Illinois, Urbana. Department of Astronomy; Estados UnidosFil: Li, Zhi Yun. University of Virginia. Astronomy Department; Estados UnidosFil: Rao, Ramprasad . Academia Sinica. Institute of Astronomy and Astrophysics; Estados UnidosNature Publishing Group2014-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/7230Stephens, Ian W. ; Looney, Leslie W. ; Kwon, Woojin ; Fernandez Lopez, Manuel; Hughes, A. Meredith ; et al.; Spatially resolved magnetic field structure in the disk of a T Tauri star; Nature Publishing Group; Nature; 154; 7524; 10-2014; 597–5990028-0836enginfo:eu-repo/semantics/altIdentifier/arxiv/http://arxiv.org/abs/1409.2878info:eu-repo/semantics/altIdentifier/url/http://www.nature.com/nature/journal/v514/n7524/full/nature13850.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1038/nature13850info:eu-repo/semantics/altIdentifier/doi/info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:33:49Zoai:ri.conicet.gov.ar:11336/7230instacron: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 09:33:49.99CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Spatially resolved magnetic field structure in the disk of a T Tauri star |
title |
Spatially resolved magnetic field structure in the disk of a T Tauri star |
spellingShingle |
Spatially resolved magnetic field structure in the disk of a T Tauri star Stephens, Ian W. Star formation Protostellar disks Polarization margnetic fields T Tauri stars |
title_short |
Spatially resolved magnetic field structure in the disk of a T Tauri star |
title_full |
Spatially resolved magnetic field structure in the disk of a T Tauri star |
title_fullStr |
Spatially resolved magnetic field structure in the disk of a T Tauri star |
title_full_unstemmed |
Spatially resolved magnetic field structure in the disk of a T Tauri star |
title_sort |
Spatially resolved magnetic field structure in the disk of a T Tauri star |
dc.creator.none.fl_str_mv |
Stephens, Ian W. Looney, Leslie W. Kwon, Woojin Fernandez Lopez, Manuel Hughes, A. Meredith Mundy, Lee G. Crutcher, Richard M. Li, Zhi Yun Rao, Ramprasad |
author |
Stephens, Ian W. |
author_facet |
Stephens, Ian W. Looney, Leslie W. Kwon, Woojin Fernandez Lopez, Manuel Hughes, A. Meredith Mundy, Lee G. Crutcher, Richard M. Li, Zhi Yun Rao, Ramprasad |
author_role |
author |
author2 |
Looney, Leslie W. Kwon, Woojin Fernandez Lopez, Manuel Hughes, A. Meredith Mundy, Lee G. Crutcher, Richard M. Li, Zhi Yun Rao, Ramprasad |
author2_role |
author author author author author author author author |
dc.subject.none.fl_str_mv |
Star formation Protostellar disks Polarization margnetic fields T Tauri stars |
topic |
Star formation Protostellar disks Polarization margnetic fields T Tauri stars |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Magnetic fields in accretion disks play a dominant role during the star formation process but have hitherto been observationally poorly constrained. Field strengths have been inferred on T Tauri stars themselves and possibly in the innermost part of the accretion disk, but the strength and morphology of the field in the bulk of the disk have not been observed. Unresolved measurements of polarized emission (arising from elongated dust grains aligned perpendicular to the field) imply average fields aligned with the disks. Theoretically, the fields are expected to be largely toroidal, poloidal, or a mixture of the two, which imply different mechanisms for transporting angular momentum in the disks of actively accreting young stars such as HL Tau. Here we report resolved measurements of the polarized 1.25 mm continuum emission from HL Tau's disk. The magnetic field on a scale of 80 AU is coincident with the major axis (~210 AU diameter) of the disk. From this we conclude that the magnetic field inside the disk at this scale cannot be dominated by a vertical component, though a purely toroidal field does not fit the data well either. The unexpected morphology suggests that the magnetic field's role for the accretion of a T Tauri star is more complex than the current theoretical understanding. Fil: Stephens, Ian W. . Boston University, Institute for Astrophysical Research; Estados Unidos Fil: Looney, Leslie W. . University of Illinois, Urbana. Department of Astronomy; Estados Unidos Fil: Kwon, Woojin . Netherlands Institute for Space Research, Groningen; Países Bajos Fil: Fernandez Lopez, Manuel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); Argentina Fil: Hughes, A. Meredith . Wesleyan University. Van Vleck Observatory, Astronomy Department ; Estados Unidos Fil: Mundy, Lee G. . University of Maryland. Astronomy Department & Laboratory for Millimeter-wave Astronomy; Estados Unidos Fil: Crutcher, Richard M. . University of Illinois, Urbana. Department of Astronomy; Estados Unidos Fil: Li, Zhi Yun. University of Virginia. Astronomy Department; Estados Unidos Fil: Rao, Ramprasad . Academia Sinica. Institute of Astronomy and Astrophysics; Estados Unidos |
description |
Magnetic fields in accretion disks play a dominant role during the star formation process but have hitherto been observationally poorly constrained. Field strengths have been inferred on T Tauri stars themselves and possibly in the innermost part of the accretion disk, but the strength and morphology of the field in the bulk of the disk have not been observed. Unresolved measurements of polarized emission (arising from elongated dust grains aligned perpendicular to the field) imply average fields aligned with the disks. Theoretically, the fields are expected to be largely toroidal, poloidal, or a mixture of the two, which imply different mechanisms for transporting angular momentum in the disks of actively accreting young stars such as HL Tau. Here we report resolved measurements of the polarized 1.25 mm continuum emission from HL Tau's disk. The magnetic field on a scale of 80 AU is coincident with the major axis (~210 AU diameter) of the disk. From this we conclude that the magnetic field inside the disk at this scale cannot be dominated by a vertical component, though a purely toroidal field does not fit the data well either. The unexpected morphology suggests that the magnetic field's role for the accretion of a T Tauri star is more complex than the current theoretical understanding. |
publishDate |
2014 |
dc.date.none.fl_str_mv |
2014-10 |
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/11336/7230 Stephens, Ian W. ; Looney, Leslie W. ; Kwon, Woojin ; Fernandez Lopez, Manuel; Hughes, A. Meredith ; et al.; Spatially resolved magnetic field structure in the disk of a T Tauri star; Nature Publishing Group; Nature; 154; 7524; 10-2014; 597–599 0028-0836 |
url |
http://hdl.handle.net/11336/7230 |
identifier_str_mv |
Stephens, Ian W. ; Looney, Leslie W. ; Kwon, Woojin ; Fernandez Lopez, Manuel; Hughes, A. Meredith ; et al.; Spatially resolved magnetic field structure in the disk of a T Tauri star; Nature Publishing Group; Nature; 154; 7524; 10-2014; 597–599 0028-0836 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/arxiv/http://arxiv.org/abs/1409.2878 info:eu-repo/semantics/altIdentifier/url/http://www.nature.com/nature/journal/v514/n7524/full/nature13850.html info:eu-repo/semantics/altIdentifier/doi/10.1038/nature13850 info:eu-repo/semantics/altIdentifier/doi/ |
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 |
Nature Publishing Group |
publisher.none.fl_str_mv |
Nature Publishing Group |
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 |
_version_ |
1844613042369724416 |
score |
13.070432 |