School of Earth and Space Sciences, Peking University, Beijing 100871, People's Republic of China.
Universities Space Research Association, Huntsville, AL 35805, USA.
Science. 2020 Aug 7;369(6504):694-697. doi: 10.1126/science.abb4462.
Understanding many physical processes in the solar atmosphere requires determination of the magnetic field in each atmospheric layer. However, direct measurements of the magnetic field in the Sun's corona are difficult to obtain. Using observations with the Coronal Multi-channel Polarimeter, we have determined the spatial distribution of the plasma density in the corona and the phase speed of the prevailing transverse magnetohydrodynamic waves within the plasma. We combined these measurements to map the plane-of-sky component of the global coronal magnetic field. The derived field strengths in the corona, from 1.05 to 1.35 solar radii, are mostly 1 to 4 gauss. Our results demonstrate the capability of imaging spectroscopy in coronal magnetic field diagnostics.
理解太阳大气层中的许多物理过程需要确定每个大气层的磁场。然而，直接测量太阳日冕中的磁场是很困难的。利用日冕多通道偏振仪的观测结果，我们已经确定了日冕中的等离子体密度的空间分布以及等离子体内占主导地位的横向磁流体动力学波的相速度。我们将这些测量结果结合起来，绘制了日球层中全球日冕磁场的天顶平面分量图。在 1.05 到 1.35 个太阳半径的范围内，日冕中的推算场强大多在 1 到 4 高斯之间。我们的结果证明了成像光谱在日冕磁场诊断中的能力。
