High-Resolution Millimeter-Wave Mapping of Linearly Polarized Dust Emission: Magnetic Field Structure in Orion
High-Resolution Millimeter-Wave Mapping of Linearly Polarized Dust Emission: Magnetic Field Structure in Orion
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DOI：
10.1086/311485
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发表时间：
1998-05
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影响因子：
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通讯作者：
R. Rao;R. Crutcher;R. Plambeck;M. C. H. W. U. I. A. Urbana;Univ. of California at Berkeley
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文献类型：
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作者：
R. Rao;R. Crutcher;R. Plambeck;M. C. H. W. U. I. A. Urbana;Univ. of California at Berkeley
我们提出了1.3和3.3毫米的偏振图的猎户座-KL获得的比马阵列在约4“的分辨率。来自磁性排列的尘埃颗粒的热辐射产生偏振。沿着猎户座“脊”，偏振位置角从10°到40°平滑变化，与以前的低分辨率地图一致。然而，在猎户座“热核心”以南的一个小区域，位置角改变了90°。这种极化方向的突然变化不一定是扭曲磁场的标志。相反，在这个局部区域，除了通常的戴维斯-格林斯坦机制之外，其他过程可能会使尘埃颗粒的长轴平行于场，垂直于它们的正常方向。
We present 1.3 and 3.3 mm polarization maps of Orion-KL obtained with the BIMA array at approximately 4'' resolution. Thermal emission from magnetically aligned dust grains produces the polarization. Along the Orion "ridge" the polarization position angle varies smoothly from about 10° to 40°, in agreement with previous lower resolution maps. In a small region south of the Orion "hot core," however, the position angle changes by 90°. This abrupt change in polarization direction is not necessarily the signpost of a twisted magnetic field. Rather, in this localized region, processes other than the usual Davis-Greenstein mechanism might align the dust grains with their long axes parallel with the field, orthogonal to their normal orientation.