Molecular outflow launched beyond the disk edge

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dc.creatorFelipe de Oliveira Alves
dc.creatorJosep Miquel Girart
dc.creatorPaola Caselli
dc.creatorGabriel Armando Pellegatti Franco
dc.creatorBo Zhao
dc.creatorWouter H. T. Vlemmings
dc.creatorMarc Graham Evans
dc.creatorLuca Ricci
dc.date.accessioned2023-09-11T19:51:28Z
dc.date.accessioned2025-09-08T23:30:13Z
dc.date.available2023-09-11T19:51:28Z
dc.date.issued2017
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Gerais
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201731077
dc.identifier.issn1432-0746
dc.identifier.urihttps://hdl.handle.net/1843/58565
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofAstronomy & Astrophysics
dc.rightsAcesso Aberto
dc.subjectEstrelas
dc.subjectAcreção
dc.subjectCampos magnéticos
dc.subject.otherStars
dc.subject.otherAccretion
dc.subject.otherMagnetic fields
dc.titleMolecular outflow launched beyond the disk edge
dc.typeArtigo de periódico
local.citation.epage5
local.citation.spage1
local.citation.volume603
local.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.
local.identifier.orcidhttps://orcid.org/0000-0002-7945-064X
local.identifier.orcidhttps://orcid.org/0000-0002-3829-5591
local.identifier.orcidhttps://orcid.org/0000-0003-1481-7911
local.identifier.orcidhttps://orcid.org/0000-0003-2020-2649
local.identifier.orcidhttps://orcid.org/0000-0002-5359-8072
local.identifier.orcidhttps://orcid.org/0000-0002-2700-9916
local.identifier.orcidhttps://orcid.org/0000-0002-1176-4378
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://www.aanda.org/articles/aa/full_html/2017/07/aa31077-17/aa31077-17.html

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