Magnetic field in a young circumbinary disk
| Autor(a) principal: | |
|---|---|
| Data de Publicação: | 2018 |
| Outros Autores: | , , , , , , , |
| Tipo de documento: | Artigo |
| Idioma: | eng |
| Título da fonte: | Repositório Institucional da UFMG |
| Texto Completo: | https://doi.org/10.1051/0004-6361/201832935 http://hdl.handle.net/1843/58562 https://orcid.org/0000-0002-7945-064X https://orcid.org/0000-0002-3829-5591 https://orcid.org/0000-0003-2303-0096 https://orcid.org/0000-0001-7706-6049 https://orcid.org/0000-0003-2020-2649 https://orcid.org/0000-0003-1481-7911 https://orcid.org/0000-0002-2700-9916 https://orcid.org/0000-0003-2384-6589 https://orcid.org/0000-0002-5135-8657 |
Resumo: | CNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico |
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2023-09-11T19:21:25Z2023-09-11T19:21:25Z201861618https://doi.org/10.1051/0004-6361/2018329351432-0746http://hdl.handle.net/1843/58562https://orcid.org/0000-0002-7945-064Xhttps://orcid.org/0000-0002-3829-5591https://orcid.org/0000-0003-2303-0096https://orcid.org/0000-0001-7706-6049https://orcid.org/0000-0003-2020-2649https://orcid.org/0000-0003-1481-7911https://orcid.org/0000-0002-2700-9916https://orcid.org/0000-0003-2384-6589https://orcid.org/0000-0002-5135-8657CNPq - Conselho Nacional de Desenvolvimento Científico e TecnológicoFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas GeraisCONTEXT: Polarized continuum emission at millimeter-to-submillimeter wavelengths is usually attributed to thermal emission from dust grains aligned through radiative torques with the magnetic field. However, recent theoretical work has shown that under specific conditions polarization may arise from self-scattering of thermal emission and by radiation fields from a nearby stellar object. AIMS: We use multi-frequency polarization observations of a circumbinary disk to investigate how the polarization properties change at distinct frequency bands. Our goal is to discern the main mechanism responsible for the polarization through comparison between our observations and model predictions for each of the proposed mechanisms. METHODS: We used the Atacama Large Millimeter/submillimeter Array to perform full polarization observations at 97.5 GHz (Band 3), 233 GHz (Band 6) and 343.5 GHz (Band 7). The ALMA data have a mean spatial resolution of 28 AU. The target is the Class I object BHB07-11, which is the youngest object in the Barnard 59 protocluster. Complementary Karl G. Jansky Very Large Array observations at 34.5 GHz were also performed and revealed a binary system at centimetric continuum emission within the disk. RESULTS: We detect an extended and structured polarization pattern that is remarkably consistent between the three bands. The dis- tribution of polarized intensity resembles a horseshoe shape with polarization angles following this morphology. From the spectral index between Bands 3 and 7, we derived a dust opacity index β ∼ 1 consistent with maximum grain sizes larger than expected to produce self-scattering polarization in each band. The polarization morphology and the polarization levels do not match predictions from self-scattering. On the other hand, marginal correspondence is seen between our maps and predictions from a radiation field model assuming the brightest binary component as main radiation source. Previous molecular line data from BHB07-11 indicates disk rotation. We used the DustPol module of the ARTIST radiative transfer tool to produce synthetic polarization maps from a rotating magnetized disk model assuming combined poloidal and toroidal magnetic field components. The magnetic field vectors (i.e., the polarization vectors rotated by 90◦) are better represented by a model with poloidal magnetic field strength about three times the toroidal one. Conclusions: The similarity of our polarization patterns among the three bands provides a strong evidence against self-scattering and radiation fields. On the other hand, our data are reasonably well reproduced by a model of disk with toroidal magnetic field components slightly smaller than poloidal ones. The residual is likely to be due to the internal twisting of the magnetic field due to the binary system dynamics, which is not considered in our model.engUniversidade Federal de Minas GeraisUFMGBrasilICX - DEPARTAMENTO DE FÍSICAAstronomy & AstrophysicsCampos magnéticosEspalhamentoPolarizaçãoMagnetic fieldsPolarizationScatteringProtoplanetary disksMagnetic field in a young circumbinary diskinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttps://www.aanda.org/articles/aa/full_html/2018/08/aa32935-18/aa32935-18.htmlFelipe de Oliveira AlvesJosep Miquel GirartMarco PadovaniDaniele GalliGabriel Armando Pellegatti FrancoPaola CaselliWouter H. T. VlemmingsQizhou ZhangHelmut Wilfried Wiesemeyerapplication/pdfinfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFMGinstname:Universidade Federal de Minas Gerais (UFMG)instacron:UFMGORIGINALMagnetic field in a young circumbinary disk.pdfMagnetic field in a young circumbinary disk.pdfapplication/pdf2026505https://repositorio.ufmg.br/bitstream/1843/58562/2/Magnetic%20field%20in%20a%20young%20circumbinary%20disk.pdfa140b6949454bf1e2b6bd5ad485f2db5MD52LICENSELicense.txtLicense.txttext/plain; charset=utf-82042https://repositorio.ufmg.br/bitstream/1843/58562/1/License.txtfa505098d172de0bc8864fc1287ffe22MD511843/585622023-09-11 18:43:24.556oai:repositorio.ufmg.br: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Repositório de PublicaçõesPUBhttps://repositorio.ufmg.br/oaiopendoar:2023-09-11T21:43:24Repositório Institucional da UFMG - Universidade Federal de Minas Gerais (UFMG)false |
| dc.title.pt_BR.fl_str_mv |
Magnetic field in a young circumbinary disk |
| title |
Magnetic field in a young circumbinary disk |
| spellingShingle |
Magnetic field in a young circumbinary disk Felipe de Oliveira Alves Magnetic fields Polarization Scattering Protoplanetary disks Campos magnéticos Espalhamento Polarização |
| title_short |
Magnetic field in a young circumbinary disk |
| title_full |
Magnetic field in a young circumbinary disk |
| title_fullStr |
Magnetic field in a young circumbinary disk |
| title_full_unstemmed |
Magnetic field in a young circumbinary disk |
| title_sort |
Magnetic field in a young circumbinary disk |
| author |
Felipe de Oliveira Alves |
| author_facet |
Felipe de Oliveira Alves Josep Miquel Girart Marco Padovani Daniele Galli Gabriel Armando Pellegatti Franco Paola Caselli Wouter H. T. Vlemmings Qizhou Zhang Helmut Wilfried Wiesemeyer |
| author_role |
author |
| author2 |
Josep Miquel Girart Marco Padovani Daniele Galli Gabriel Armando Pellegatti Franco Paola Caselli Wouter H. T. Vlemmings Qizhou Zhang Helmut Wilfried Wiesemeyer |
| author2_role |
author author author author author author author author |
| dc.contributor.author.fl_str_mv |
Felipe de Oliveira Alves Josep Miquel Girart Marco Padovani Daniele Galli Gabriel Armando Pellegatti Franco Paola Caselli Wouter H. T. Vlemmings Qizhou Zhang Helmut Wilfried Wiesemeyer |
| dc.subject.por.fl_str_mv |
Magnetic fields Polarization Scattering Protoplanetary disks |
| topic |
Magnetic fields Polarization Scattering Protoplanetary disks Campos magnéticos Espalhamento Polarização |
| dc.subject.other.pt_BR.fl_str_mv |
Campos magnéticos Espalhamento Polarização |
| description |
CNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico |
| publishDate |
2018 |
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2018 |
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2023-09-11T19:21:25Z |
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2023-09-11T19:21:25Z |
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info:eu-repo/semantics/publishedVersion |
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info:eu-repo/semantics/article |
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http://hdl.handle.net/1843/58562 |
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https://doi.org/10.1051/0004-6361/201832935 |
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1432-0746 |
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https://orcid.org/0000-0002-7945-064X https://orcid.org/0000-0002-3829-5591 https://orcid.org/0000-0003-2303-0096 https://orcid.org/0000-0001-7706-6049 https://orcid.org/0000-0003-2020-2649 https://orcid.org/0000-0003-1481-7911 https://orcid.org/0000-0002-2700-9916 https://orcid.org/0000-0003-2384-6589 https://orcid.org/0000-0002-5135-8657 |
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1432-0746 |
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eng |
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Astronomy & Astrophysics |
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Universidade Federal de Minas Gerais |
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Brasil |
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ICX - DEPARTAMENTO DE FÍSICA |
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Universidade Federal de Minas Gerais |
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