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dc.contributor.authorPoidevin, F.
dc.contributor.authorFalceta-Gonçalves, D.
dc.contributor.authorKowal, G.
dc.contributor.authorDe Gouveia Dal Pino, E.
dc.contributor.authorMagalhães, A.M.
dc.date.accessioned2014-09-25T12:01:04Z
dc.date.available2014-09-25T12:01:04Z
dc.date.issued2013-11-10
dc.identifier.citationPoidevin , F , Falceta-Gonçalves , D , Kowal , G , De Gouveia Dal Pino , E & Magalhães , A M 2013 , ' Magnetic field components analysis of the SCUPOL 850 μm polarization data catalog ' , Astrophysical Journal , vol. 777 , no. 2 , 112 . https://doi.org/10.1088/0004-637X/777/2/112en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 151129145
dc.identifier.otherPURE UUID: 88d06e7a-28bf-4a34-b4ad-e24336799539
dc.identifier.otherScopus: 84886694703
dc.identifier.urihttp://hdl.handle.net/10023/5498
dc.descriptionD.F.G. thanks the European Research Council (ADG-2011 ECOGAL), and brazilian agencies CNPq (No. 300382/2008-1), CAPES (3400-13-1) and FAPESP (No. 2011/12909-8) for financial support.en
dc.description.abstractWe present an extensive analysis of the 850 μm polarization maps of the SCUBA Polarimeter Legacy (SCUPOL) Catalogue produced by Matthews et al., focusing exclusively on the molecular clouds and star-forming regions. For the sufficiently sampled regions, we characterize the depolarization properties and the turbulent-to-mean magnetic field ratio of each region. Similar sets of parameters are calculated from two-dimensional synthetic maps of dust-emission polarization produced with three-dimensional magnetohydrodynamics (MHD) numerical simulations scaled to the S106, OMC-2/3, W49, and DR21 molecular cloud polarization maps. For these specific regions, the turbulent MHD regimes retrieved from the simulations, as described by the turbulent Alfvén and Sonic Mach numbers, are consistent within a factor one to two with the values of the same turbulent regimes estimated from the analysis of Zeeman measurements data provided by Crutcher. Constraints on the values of the inclination angle α of the mean magnetic field with respect to the line of sight are also given. The values obtained from the comparison of the simulations with the SCUPOL data are consistent with the estimates made by using two observational methods provided by other authors. Our main conclusion is that simple, ideal, isothermal, and non-self-gravitating MHD simulations are sufficient in order to describe the large-scale observed physical properties of the envelopes of this set of regions.
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2013. The American Astronomical Society. All rights reserved.en
dc.subjectISM: cloudsen
dc.subjectISM: individual objects: SCUPOLen
dc.subjectISM: structureen
dc.subjectMagnetic fieldsen
dc.subjectPolarizationen
dc.subjectSubmillimeter: ISMen
dc.subjectTurbulenceen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleMagnetic field components analysis of the SCUPOL 850 μm polarization data catalogen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Research Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/777/2/112
dc.description.statusPeer revieweden
dc.identifier.grantnumberen


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