Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?

Autores
Harrison, Rachel E.; Lin, Zhe-Yu Daniel; Looney, Leslie W.; Li, Zhi-Yun; Yang, Haifeng; Stephens, Ian W.; Fernández López, Manuel
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Millimeter and submillimeter observations of continuum linear dust polarization provide insight into dust grain growth in protoplanetary disks, which are the progenitors of planetary systems. We present the results of the first survey of dust polarization in protoplanetary disks at 870 μm and 3 mm. We find that protoplanetary disks in the same molecular cloud at similar evolutionary stages can exhibit different correlations between observing wavelength and polarization morphology and fraction. We explore possible origins for these differences in polarization, including differences in dust populations and protostar properties. For RY Tau and MWC 480, which are consistent with scattering at both wavelengths, we present models of the scattering polarization from several dust grain size distributions. These models aim to reproduce two features of the observational results for these disks: (1) both disks have an observable degree of polarization at both wavelengths; and (2) the polarization fraction is higher at 3 mm than at 870 μm in the centers of the disks. For both disks, these features can be reproduced by a power-law distribution of spherical dust grains with a maximum radius of 200 μm and high optical depth. In MWC 480, we can also reproduce features (1) and (2) with a model containing large grains (amax = 490 μm) near the disk midplane and small grains (amax = 140 μm) above and below the midplane.
Instituto Argentino de Radioastronomía
Materia
Ciencias Astronómicas
Protoplanetary disks
Polarimetry
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/167344

id SEDICI_75f8a6daaee84432e51b9e3a2ca5132c
oai_identifier_str oai:sedici.unlp.edu.ar:10915/167344
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?Harrison, Rachel E.Lin, Zhe-Yu DanielLooney, Leslie W.Li, Zhi-YunYang, HaifengStephens, Ian W.Fernández López, ManuelCiencias AstronómicasProtoplanetary disksPolarimetryMillimeter and submillimeter observations of continuum linear dust polarization provide insight into dust grain growth in protoplanetary disks, which are the progenitors of planetary systems. We present the results of the first survey of dust polarization in protoplanetary disks at 870 μm and 3 mm. We find that protoplanetary disks in the same molecular cloud at similar evolutionary stages can exhibit different correlations between observing wavelength and polarization morphology and fraction. We explore possible origins for these differences in polarization, including differences in dust populations and protostar properties. For RY Tau and MWC 480, which are consistent with scattering at both wavelengths, we present models of the scattering polarization from several dust grain size distributions. These models aim to reproduce two features of the observational results for these disks: (1) both disks have an observable degree of polarization at both wavelengths; and (2) the polarization fraction is higher at 3 mm than at 870 μm in the centers of the disks. For both disks, these features can be reproduced by a power-law distribution of spherical dust grains with a maximum radius of 200 μm and high optical depth. In MWC 480, we can also reproduce features (1) and (2) with a model containing large grains (amax = 490 μm) near the disk midplane and small grains (amax = 140 μm) above and below the midplane.Instituto Argentino de Radioastronomía2024info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/167344enginfo:eu-repo/semantics/altIdentifier/issn/1538-4357info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad39ecinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:44:35Zoai:sedici.unlp.edu.ar:10915/167344Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:44:35.792SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
title Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
spellingShingle Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
Harrison, Rachel E.
Ciencias Astronómicas
Protoplanetary disks
Polarimetry
title_short Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
title_full Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
title_fullStr Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
title_full_unstemmed Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
title_sort Protoplanetary Disk Polarization at Multiple Wavelengths: Are Dust Populations Diverse?
dc.creator.none.fl_str_mv Harrison, Rachel E.
Lin, Zhe-Yu Daniel
Looney, Leslie W.
Li, Zhi-Yun
Yang, Haifeng
Stephens, Ian W.
Fernández López, Manuel
author Harrison, Rachel E.
author_facet Harrison, Rachel E.
Lin, Zhe-Yu Daniel
Looney, Leslie W.
Li, Zhi-Yun
Yang, Haifeng
Stephens, Ian W.
Fernández López, Manuel
author_role author
author2 Lin, Zhe-Yu Daniel
Looney, Leslie W.
Li, Zhi-Yun
Yang, Haifeng
Stephens, Ian W.
Fernández López, Manuel
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Protoplanetary disks
Polarimetry
topic Ciencias Astronómicas
Protoplanetary disks
Polarimetry
dc.description.none.fl_txt_mv Millimeter and submillimeter observations of continuum linear dust polarization provide insight into dust grain growth in protoplanetary disks, which are the progenitors of planetary systems. We present the results of the first survey of dust polarization in protoplanetary disks at 870 μm and 3 mm. We find that protoplanetary disks in the same molecular cloud at similar evolutionary stages can exhibit different correlations between observing wavelength and polarization morphology and fraction. We explore possible origins for these differences in polarization, including differences in dust populations and protostar properties. For RY Tau and MWC 480, which are consistent with scattering at both wavelengths, we present models of the scattering polarization from several dust grain size distributions. These models aim to reproduce two features of the observational results for these disks: (1) both disks have an observable degree of polarization at both wavelengths; and (2) the polarization fraction is higher at 3 mm than at 870 μm in the centers of the disks. For both disks, these features can be reproduced by a power-law distribution of spherical dust grains with a maximum radius of 200 μm and high optical depth. In MWC 480, we can also reproduce features (1) and (2) with a model containing large grains (amax = 490 μm) near the disk midplane and small grains (amax = 140 μm) above and below the midplane.
Instituto Argentino de Radioastronomía
description Millimeter and submillimeter observations of continuum linear dust polarization provide insight into dust grain growth in protoplanetary disks, which are the progenitors of planetary systems. We present the results of the first survey of dust polarization in protoplanetary disks at 870 μm and 3 mm. We find that protoplanetary disks in the same molecular cloud at similar evolutionary stages can exhibit different correlations between observing wavelength and polarization morphology and fraction. We explore possible origins for these differences in polarization, including differences in dust populations and protostar properties. For RY Tau and MWC 480, which are consistent with scattering at both wavelengths, we present models of the scattering polarization from several dust grain size distributions. These models aim to reproduce two features of the observational results for these disks: (1) both disks have an observable degree of polarization at both wavelengths; and (2) the polarization fraction is higher at 3 mm than at 870 μm in the centers of the disks. For both disks, these features can be reproduced by a power-law distribution of spherical dust grains with a maximum radius of 200 μm and high optical depth. In MWC 480, we can also reproduce features (1) and (2) with a model containing large grains (amax = 490 μm) near the disk midplane and small grains (amax = 140 μm) above and below the midplane.
publishDate 2024
dc.date.none.fl_str_mv 2024
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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://sedici.unlp.edu.ar/handle/10915/167344
url http://sedici.unlp.edu.ar/handle/10915/167344
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/1538-4357
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad39ec
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
_version_ 1844616312820596736
score 13.070432