Magnetically dominated parallel interstellar filaments in the infrared dark cloud G14.225-0.506

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dc.creatorFábio Pereira Santos
dc.creatorGemma Busquet Rico
dc.creatorGabriel Armando Pellegatti Franco
dc.creatorJosep Miquel Girart
dc.creatorQizhou Zhang
dc.date.accessioned2023-09-11T15:50:57Z
dc.date.accessioned2025-09-08T23:00:35Z
dc.date.available2023-09-11T15:50:57Z
dc.date.issued2016
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Gerais
dc.description.sponsorshipCAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível Superior
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.3847/0004-637X/832/2/186
dc.identifier.issn1538-4357
dc.identifier.urihttps://hdl.handle.net/1843/58549
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofThe Astrophysical Journal
dc.rightsAcesso Aberto
dc.subjectCampos magnéticos
dc.subjectPolarimetria
dc.subjectMeio interestelar
dc.subject.otherStars
dc.titleMagnetically dominated parallel interstellar filaments in the infrared dark cloud G14.225-0.506
dc.typeArtigo de periódico
local.citation.epage15
local.citation.issue2
local.citation.spage1
local.citation.volume832
local.description.resumoThe infrared dark cloud G14.225-0.506 (IRDC G14.2) displays a remarkable complex of parallel dense molecular filaments projected on the plane of the sky. Previous studies of dust emission and molecular lines have speculated whether magnetic fields could have played an important role in the formation of such elongated structures, which are hosts to numerous young stellar sources. In this work we have conducted a vast polarimetric survey at optical and near-infrared wavelengths in order to study the morphology of magnetic field lines in IRDC G14.2 through the observation of background stars. The orientation of interstellar polarization, which traces magnetic field lines, is perpendicular to most of the filamentary features within the cloud. Additionally, the larger-scale molecular cloud as a whole exhibits an elongated shape also perpendicular to magnetic fields. Estimates of magnetic field strengths indicate values in the range 320–550 μG, which allow sub-alfvénic conditions, but do not prevent the gravitational collapse of hub–filament structures, which in general are close to the critical state. These characteristics suggest that magnetic fields played the main role in regulating the collapse from large to small scales, leading to the formation of series of parallel elongated structures. The morphology is also consistent with numerical simulations that show how gravitational instabilities develop when subjected to strong magnetic fields. Finally, the results corroborate the hypothesis that strong support from internal magnetic fields might explain why the cloud seems to be contracting on a timescale 2–3 times longer than what is expected from a free-fall collapse.
local.identifier.orcidhttps://orcid.org/0000-0002-9650-3619
local.identifier.orcidhttps://orcid.org/0000-0002-2189-6278
local.identifier.orcidhttps://orcid.org/0000-0002-3829-5591
local.identifier.orcidhttps://orcid.org/0000-0003-2384-6589
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://iopscience.iop.org/article/10.3847/0004-637X/832/2/186

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