期刊
ASTROPHYSICAL JOURNAL
卷 704, 期 2, 页码 891-897出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/704/2/891
关键词
ISM: clouds; ISM: magnetic fields; polarization; stars: formation; turbulence
资金
- Smithsonian Astrophysics Observatory
- NSF [AST-0505124, AST-0540882]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908159] Funding Source: National Science Foundation
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.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据