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Please use this identifier to cite or link to this item: http://hdl.handle.net/1843/58565
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dc.creatorFelipe de Oliveira Alvespt_BR
dc.creatorJosep Miquel Girartpt_BR
dc.creatorPaola Casellipt_BR
dc.creatorGabriel Armando Pellegatti Francopt_BR
dc.creatorBo Zhaopt_BR
dc.creatorWouter H. T. Vlemmingspt_BR
dc.creatorMarc Graham Evanspt_BR
dc.creatorLuca Riccipt_BR
dc.date.accessioned2023-09-11T19:51:28Z-
dc.date.available2023-09-11T19:51:28Z-
dc.date.issued2017-
dc.citation.volume603pt_BR
dc.citation.spage1pt_BR
dc.citation.epage5pt_BR
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201731077pt_BR
dc.identifier.issn1432-0746pt_BR
dc.identifier.urihttp://hdl.handle.net/1843/58565-
dc.description.resumoOne of the long-standing problems of star formation is the excess of angular momentum of the parent molecular cloud. In the classical picture, a fraction of angular momentum of the circumstellar material is removed by the magneto-centrifugally driven disk wind that is launched from a wide region throughout the disk. In this work, we investigate the kinematics in the envelope-disk transition zone of the Class I object BHB07-11, in the B59 core. For this purpose, we used the Atacama Large Millimeter/submillimeter Array in extended configuration to observe the thermal dust continuum emission (λ0 ~ 1.3 mm) and molecular lines (CO, C18O and H2CO), which are suitable tracers of disk, envelope, and outflow dynamics at a spatial resolution of ~30 AU. We report a bipolar outflow that was launched at symmetric positions with respect to the disk (~80 AU in radius), but was concentrated at a distance of 90–130 AU from the disk center. The two outflow lobes had a conical shape and the gas inside was accelerating. The large offset of the launching position coincided with the landing site of the infall materials from the extended spiral structure (seen in dust) onto the disk. This indicates that bipolar outflows are efficiently launched within a narrow region outside the disk edge. We also identify a sharp transition in the gas kinematics across the tip of the spiral structure, which pinpoints the location of the so-called centrifugal barrier.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.subjectStarspt_BR
dc.subjectAccretionpt_BR
dc.subjectMagnetic fieldspt_BR
dc.subject.otherEstrelaspt_BR
dc.subject.otherAcreçãopt_BR
dc.subject.otherCampos magnéticospt_BR
dc.titleMolecular outflow launched beyond the disk edgept_BR
dc.typeArtigo de Periódicopt_BR
dc.url.externahttps://www.aanda.org/articles/aa/full_html/2017/07/aa31077-17/aa31077-17.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/0000-0003-1481-7911pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0003-2020-2649pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-5359-8072pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-2700-9916pt_BR
dc.identifier.orcidhttps://orcid.org/0000-0002-1176-4378pt_BR
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