1.3 mm Polarized emission in the circumstellar disk of a massive protostar

Autores
Fernandez Lopez, Manuel; Stephens, I. W.; Girart, J. M.; Looney, L.; Curiel, S.; Segura Cox, D.; Eswaraiah, C.; Lai, S. P.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present the first resolved observations of the 1.3 mm polarized emission from the disk-like structure surrounding the high-mass protostar Cepheus A HW2. These CARMA data partially resolve the dust polarization, suggesting a uniform morphology of polarization vectors with an average position angle of 57° ± 6° and an average polarization fraction of 2.0% ± 0.4%. The distribution of the polarization vectors can be attributed to (1) the direct emission of magnetically aligned grains of dust by a uniform magnetic field, or (2) the pattern produced by the scattering of an inclined disk. We show that both models can explain the observations, and perhaps a combination of the two mechanisms produces the polarized emission. A third model including a toroidal magnetic field does not match the observations. Assuming scattering is the polarization mechanism, these observations suggest that during the first few 104 years of high-mass star formation, grain sizes can grow from1 mm to several 10s μm.
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina
Fil: Stephens, I. W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Boston University; Estados Unidos. University of Illinois; Estados Unidos
Fil: Girart, J. M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Institut de Ciències de l’Espai; España
Fil: Looney, L.. University of Illinois; Estados Unidos
Fil: Curiel, S.. Universidad Nacional Autónoma de México; México
Fil: Segura Cox, D.. University of Illinois; Estados Unidos
Fil: Eswaraiah, C.. National Tsing Hua University; República de China
Fil: Lai, S. P.. National Tsing Hua University; República de China
Materia
CEPHEUS A HW2
Magnetic fields
Polarization
Formation of stars
Polarimetry
Interstellar medium
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:11336/26070
Acceder
id CONICETDig_b14b4d86e7b099dad6026d680268619f
oai_identifier_str oai:ri.conicet.gov.ar:11336/26070
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling 1.3 mm Polarized emission in the circumstellar disk of a massive protostarFernandez Lopez, ManuelStephens, I. W.Girart, J. M.Looney, L.Curiel, S.Segura Cox, D.Eswaraiah, C.Lai, S. P.CEPHEUS A HW2Magnetic fieldsPolarizationFormation of starsPolarimetryInterstellar mediumhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present the first resolved observations of the 1.3 mm polarized emission from the disk-like structure surrounding the high-mass protostar Cepheus A HW2. These CARMA data partially resolve the dust polarization, suggesting a uniform morphology of polarization vectors with an average position angle of 57° ± 6° and an average polarization fraction of 2.0% ± 0.4%. The distribution of the polarization vectors can be attributed to (1) the direct emission of magnetically aligned grains of dust by a uniform magnetic field, or (2) the pattern produced by the scattering of an inclined disk. We show that both models can explain the observations, and perhaps a combination of the two mechanisms produces the polarized emission. A third model including a toroidal magnetic field does not match the observations. Assuming scattering is the polarization mechanism, these observations suggest that during the first few 104 years of high-mass star formation, grain sizes can grow from1 mm to several 10s μm.Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; ArgentinaFil: Stephens, I. W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Boston University; Estados Unidos. University of Illinois; Estados UnidosFil: Girart, J. M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Institut de Ciències de l’Espai; EspañaFil: Looney, L.. University of Illinois; Estados UnidosFil: Curiel, S.. Universidad Nacional Autónoma de México; MéxicoFil: Segura Cox, D.. University of Illinois; Estados UnidosFil: Eswaraiah, C.. National Tsing Hua University; República de ChinaFil: Lai, S. P.. National Tsing Hua University; República de ChinaIOP Publishing2016-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/26070Fernandez Lopez, Manuel; Stephens, I. W.; Girart, J. M.; Looney, L.; Curiel, S.; et al.; 1.3 mm Polarized emission in the circumstellar disk of a massive protostar; IOP Publishing; Astrophysical Journal; 832; 2; 12-2016; 1-90004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/832/2/200info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/0004-637X/832/2/200/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:00:00Zoai:ri.conicet.gov.ar:11336/26070instacron: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 10:00:00.462CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
title 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
spellingShingle 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
Fernandez Lopez, Manuel
CEPHEUS A HW2
Magnetic fields
Polarization
Formation of stars
Polarimetry
Interstellar medium
title_short 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
title_full 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
title_fullStr 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
title_full_unstemmed 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
title_sort 1.3 mm Polarized emission in the circumstellar disk of a massive protostar
dc.creator.none.fl_str_mv Fernandez Lopez, Manuel
Stephens, I. W.
Girart, J. M.
Looney, L.
Curiel, S.
Segura Cox, D.
Eswaraiah, C.
Lai, S. P.
author Fernandez Lopez, Manuel
author_facet Fernandez Lopez, Manuel
Stephens, I. W.
Girart, J. M.
Looney, L.
Curiel, S.
Segura Cox, D.
Eswaraiah, C.
Lai, S. P.
author_role author
author2 Stephens, I. W.
Girart, J. M.
Looney, L.
Curiel, S.
Segura Cox, D.
Eswaraiah, C.
Lai, S. P.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv CEPHEUS A HW2
Magnetic fields
Polarization
Formation of stars
Polarimetry
Interstellar medium
topic CEPHEUS A HW2
Magnetic fields
Polarization
Formation of stars
Polarimetry
Interstellar medium
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present the first resolved observations of the 1.3 mm polarized emission from the disk-like structure surrounding the high-mass protostar Cepheus A HW2. These CARMA data partially resolve the dust polarization, suggesting a uniform morphology of polarization vectors with an average position angle of 57° ± 6° and an average polarization fraction of 2.0% ± 0.4%. The distribution of the polarization vectors can be attributed to (1) the direct emission of magnetically aligned grains of dust by a uniform magnetic field, or (2) the pattern produced by the scattering of an inclined disk. We show that both models can explain the observations, and perhaps a combination of the two mechanisms produces the polarized emission. A third model including a toroidal magnetic field does not match the observations. Assuming scattering is the polarization mechanism, these observations suggest that during the first few 104 years of high-mass star formation, grain sizes can grow from1 mm to several 10s μm.
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina
Fil: Stephens, I. W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Boston University; Estados Unidos. University of Illinois; Estados Unidos
Fil: Girart, J. M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Institut de Ciències de l’Espai; España
Fil: Looney, L.. University of Illinois; Estados Unidos
Fil: Curiel, S.. Universidad Nacional Autónoma de México; México
Fil: Segura Cox, D.. University of Illinois; Estados Unidos
Fil: Eswaraiah, C.. National Tsing Hua University; República de China
Fil: Lai, S. P.. National Tsing Hua University; República de China
description We present the first resolved observations of the 1.3 mm polarized emission from the disk-like structure surrounding the high-mass protostar Cepheus A HW2. These CARMA data partially resolve the dust polarization, suggesting a uniform morphology of polarization vectors with an average position angle of 57° ± 6° and an average polarization fraction of 2.0% ± 0.4%. The distribution of the polarization vectors can be attributed to (1) the direct emission of magnetically aligned grains of dust by a uniform magnetic field, or (2) the pattern produced by the scattering of an inclined disk. We show that both models can explain the observations, and perhaps a combination of the two mechanisms produces the polarized emission. A third model including a toroidal magnetic field does not match the observations. Assuming scattering is the polarization mechanism, these observations suggest that during the first few 104 years of high-mass star formation, grain sizes can grow from1 mm to several 10s μm.
publishDate 2016
dc.date.none.fl_str_mv 2016-12
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/11336/26070
Fernandez Lopez, Manuel; Stephens, I. W.; Girart, J. M.; Looney, L.; Curiel, S.; et al.; 1.3 mm Polarized emission in the circumstellar disk of a massive protostar; IOP Publishing; Astrophysical Journal; 832; 2; 12-2016; 1-9
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/26070
identifier_str_mv Fernandez Lopez, Manuel; Stephens, I. W.; Girart, J. M.; Looney, L.; Curiel, S.; et al.; 1.3 mm Polarized emission in the circumstellar disk of a massive protostar; IOP Publishing; Astrophysical Journal; 832; 2; 12-2016; 1-9
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/doi/10.3847/0004-637X/832/2/200
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/0004-637X/832/2/200/meta
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
_version_ 1844613776370827264
score 13.070432

Publicaciones similares