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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/58562
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dc.creatorFelipe de Oliveira Alvespt_BR
dc.creatorJosep Miquel Girartpt_BR
dc.creatorMarco Padovanipt_BR
dc.creatorDaniele Gallipt_BR
dc.creatorGabriel Armando Pellegatti Francopt_BR
dc.creatorPaola Casellipt_BR
dc.creatorWouter H. T. Vlemmingspt_BR
dc.creatorQizhou Zhangpt_BR
dc.creatorHelmut Wilfried Wiesemeyerpt_BR
dc.date.accessioned2023-09-11T19:21:25Z-
dc.date.available2023-09-11T19:21:25Z-
dc.date.issued2018-
dc.citation.volume616pt_BR
dc.citation.spage1pt_BR
dc.citation.epage8pt_BR
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201832935pt_BR
dc.identifier.issn1432-0746pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/58562-
dc.description.resumoCONTEXT: 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.pt_BR
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológicopt_BR
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Geraispt_BR
dc.format.mimetypepdfpt_BR
dc.languageengpt_BR
dc.publisherUniversidade Federal de Minas Geraispt_BR
dc.publisher.countryBrasilpt_BR
dc.publisher.departmentICX - DEPARTAMENTO DE FÍSICApt_BR
dc.publisher.initialsUFMGpt_BR
dc.relation.ispartofAstronomy & Astrophysics-
dc.rightsAcesso Abertopt_BR
dc.subjectMagnetic fieldspt_BR
dc.subjectPolarizationpt_BR
dc.subjectScatteringpt_BR
dc.subjectProtoplanetary diskspt_BR
dc.subject.otherCampos magnéticospt_BR
dc.subject.otherEspalhamentopt_BR
dc.subject.otherPolarizaçãopt_BR
dc.titleMagnetic field in a young circumbinary diskpt_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://www.aanda.org/articles/aa/full_html/2018/08/aa32935-18/aa32935-18.htmlpt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-7945-064Xpt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-3829-5591pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-2303-0096pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0001-7706-6049pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-2020-2649pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-1481-7911pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2700-9916pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-2384-6589pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5135-8657pt_BR
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