Anchoring Magnetic Fields in Turbulent Molecular Clouds

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Anchoring Magnetic Fields in Turbulent Molecular Clouds

Show simple item record Li, Hua-bai Dowell, C. Darren Goodman, Alyssa A. Hildebrand, Roger Novak, Giles 2010-07-15T13:15:30Z 2009
dc.identifier.citation Li, Hua-bai, C. Darren Dowell, Alyssa A. Goodman, Roger Hildebrand, and Giles Novak. 2009. Anchoring magnetic fields in turbulent molecular clouds. Astrophysical Journal 704(2): 891-897. en_US
dc.identifier.issn 0004-637X en_US
dc.description.abstract One of the key problems in star formation research is to determine the role of magnetic fields. Starting from the atomic intercloud medium which has density \(n_H \sim \ 1 \ cm^{–3}\), gas must accumulate from a volume several hundred pc across in order to form a typical molecular cloud. Star formation usually occurs in cloud cores, which have linear sizes below 1 pc and densities \(n_{H2} > 10^5 \ cm^{–3}\). With current technologies, it is hard to probe magnetic fields at scales lying between the accumulation length and the size of cloud cores, a range corresponds to many levels of turbulent eddy cascade, and many orders of magnitude of density amplification. For field directions detected from the two extremes, however, we show here that a significant correlation is found. Comparing this result with molecular cloud simulations, only the sub-Alfvénic cases result in field orientations consistent with our observations. en_US
dc.description.sponsorship Astronomy en_US
dc.language.iso en_US en_US
dc.publisher American Astronomical Society en_US
dc.relation.isversionof doi:10.1088/0004-637X/704/2/891 en_US
dash.license OAP
dc.subject ISM: clouds en_US
dc.subject ISM: magnetic fields en_US
dc.subject polarization en_US
dc.subject stars: formation en_US
dc.subject turbulence en_US
dc.title Anchoring Magnetic Fields in Turbulent Molecular Clouds en_US
dc.type Journal Article en_US
dc.description.version Accepted Manuscript en_US
dc.relation.journal Astrophysical Journal en_US Goodman, Alyssa A. 2010-07-15T13:15:30Z

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