期刊
ASTROPHYSICAL JOURNAL
卷 721, 期 1, 页码 815-827出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/721/1/815
关键词
ISM: clouds; ISM: individual objects (W51 e2/e8, Orion BN/KL); ISM: magnetic fields; methods: statistical; polarization; turbulence
资金
- NSC [NSC98-2119-M-001-024-MY4]
Polarization data from high-mass star formation regions (W51 e2/e8, Orion BN/KL) are used to derive statistical properties of the plane of sky projected magnetic field. Structure function and auto-correlation function are calculated for observations with various resolutions from the BIMA and SMA interferometers, covering a range in physical scales from similar to 70 mpc to similar to 2.1 mpc. Results for the magnetic field turbulent dispersion, its turbulent-to-mean field strength ratio, and the large-scale polarization angle correlation length are presented as a function of the physical scale at the star formation sites. Power-law scaling relations emerge for some of these physical quantities. The turbulent-to-mean field strength ratio is found to be close to constant over the sampled observing range, with a hint of a decrease toward smaller scales, indicating that the role of the magnetic field and turbulence is evolving with the physical scale. A statistical method is proposed to separate large-and small-scale correlations from an initial ensemble of polarization segments. This also leads to a definition of a turbulent polarization angle correlation length.
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