论文标题
总太阳日食观测的冠状磁场拓扑
Coronal Magnetic Field Topology From Total Solar Eclipse Observations
论文作者
论文摘要
测量太阳能电晕的全球磁场仍然极具挑战性。目前，在太阳日食（TSES）中拍摄的白光图像中观察到的细尺度密度结构目前是推断电晕中的磁场方向从太阳能四肢推出到几个太阳半径（RS）的最佳代理。我们首次介绍冠状磁场的拓扑结合在1至6 rs之间，这是14个独特的Eclipse Coronae的滚动Hough Transform（RHT）的定量推断，这些冠状冠层几乎跨越了几乎两个完整的太阳能周期。我们发现，直到至少3 rs，冠状磁场的方向才变成径向，在太阳周期的不同纬度和相位，高方差在1.5至3 rs之间。我们发现，最非冠状的冠状场拓扑发生在光球中的磁场强度较弱的区域上方，而更强的光谱场与电晕中高度径向的田间线相关。此外，我们发现有大量的田间线从太阳能表面连续延伸到所有纬度的几个太阳半径，而不论存在冠状孔。这些结果对测试和限制的冠状磁场模型具有影响，以及将原位太阳风测量与太阳的来源联系起来。
Measuring the global magnetic field of the solar corona remains exceptionally challenging. The fine-scale density structures observed in white light images taken during Total Solar Eclipses (TSEs) are currently the best proxy for inferring the magnetic field direction in the corona from the solar limb out to several solar radii (Rs). We present, for the first time, the topology of the coronal magnetic field continuously between 1 and 6 Rs, as quantitatively inferred with the Rolling Hough Transform (RHT) for 14 unique eclipse coronae that span almost two complete solar cycles. We find that the direction of the coronal magnetic field does not become radial until at least 3 Rs, with a high variance between 1.5 and 3 Rs at different latitudes and phases of the solar cycle. We find that the most non-radial coronal field topologies occur above regions with weaker magnetic field strengths in the photosphere, while stronger photospheric fields are associated with highly radial field lines in the corona. In addition, we find an abundance of field lines which extend continuously from the solar surface out to several solar radii at all latitudes, regardless of the presence of coronal holes. These results have implications for testing and constraining coronal magnetic field models, and for linking in situ solar wind measurements to their sources at the Sun.
