ANCHORING MAGNETIC FIELD IN TURBULENT MOLECULAR CLOUDS

被引：23

作者：

Li, Hua-Bai ^{[1
]}

Dowell, C. Darren ^{[2
,6
]}

Goodman, Alyssa ^{[1
]}

Hildebrand, Roger ^{[3
,4
,7
]}

Novak, Giles ^{[5
]}

机构：

[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[2] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[3] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[4] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[5] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA

[6] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA

[7] Univ Chicago, Dept Phys, Chicago, IL 60637 USA

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 704卷 / 02期

基金：

美国国家科学基金会;

关键词：

ISM: clouds; ISM: magnetic fields; polarization; stars: formation; turbulence; SUBMILLIMETER POLARIZATION; STAR-FORMATION; CORES; ALIGNMENT; DENSITY; REGIONS; MODELS; DR21;

D O I：

10.1088/0004-637X/704/2/891

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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) similar to 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-Alfvenic cases result in field orientations consistent with our observations.

引用

页码：891 / 897

页数：7

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