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Scattering And Absorption of Light in Planetary Regoliths
Published on: July 1, 2019
星际气体中低马赫数流是由无线电极化梯度揭示的
B M Gaensler1, M Haverkorn, B Burkhart
1Sydney Institute for Astronomy, School of Physics, The University of Sydney, New South Wales 2006, Australia. bryan.gaensler@sydney.edu.au
Nature
|October 7, 2011
概括
研究人员对银河系的磁性流进行了成像.
科学领域:
- 天体物理学 天体物理学
- 等离子体物理学的物理学
- 星际媒介研究 星际媒介研究
背景情况:
- 星际介质 (ISM) 是一个复杂的,多相的,磁化的,动荡的环境.
- 描述星际流,包括其声波马赫数,至关重要,但由于分辨率限制,具有挑战性.
- 在无线电发射中观察到不寻常的极化结构,但它们的物理意义仍然不清楚.
研究的目的:
- 开发一种用于可视化和量化ISM扩散电离气体中磁性流的新方法.
- 为了确定星际流的基本参数,例如声波马赫数.
主要方法:
- 从无线电极化观测中分析斯托克斯向量的梯度 (Q,U).
- 观测数据与磁动力学 (MHD) 模拟星际流的比较.
- 开发用于分析极化梯度的统计工具.
主要成果:
- 斯托克斯向量的梯度揭示了一个丝状网络结构,表明磁化流.
- 与模拟的比较表明,在温暖的电离介质中,流的低声波马赫数 (M(s) 2 .
- 该方法成功地绘制了与流相关的气体密度和磁场中不连续性的图像.
结论:
- 极化无线电辐射的梯度提供了一种强大的新工具,用于图像磁化流在ISM.
- 在温暖的电离介质中星际流的特点是低声波马赫数.
- 这种技术将能够准确地确定关键的流参数 (马赫数,雷诺兹数,磁场强度).
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