The magnetic field in the Sun's corona The solar corona is the outermost layer of the Sun's atmosphere, consisting of hot, diffuse, and highly ionized plasma. The magnetic field in this region is expected to drive many of its physical properties but has been difficult to measure with observations. Yang et al. used near-infrared imaging spectroscopy to determine the electron density and magnetohydrodynamic wave speed in the corona. By combining these measurements, they derived maps of the magnetic field throughout the entire observable corona. The method could potentially be used to produce routine magnetic field maps for the corona that are similar to those already available for the Sun's surface. Science, this issue p. 694 Near-infrared observations are used to map the magnetic field across the Sun’s entire observable corona. 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.

中文翻译：

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日冕磁场的全球地图


太阳日冕中的磁场 日冕是太阳大气层的最外层，由热、扩散和高度电离的等离子体组成。该区域的磁场预计会驱动其许多物理特性，但很难通过观测来测量。杨等人。使用近红外成像光谱来确定日冕中的电子密度和磁流体动力波速。通过结合这些测量结果，他们得出了整个可观测日冕的磁场图。该方法有可能用于生成日冕的常规磁场图，类似于太阳表面现有的磁场图。科学，本期第 14 页。 694 近红外观测用于绘制太阳整个可观测日冕的磁场图。了解太阳大气中的许多物理过程需要确定每个大气层中的磁场。然而，很难直接测量太阳日冕的磁场。利用日冕多通道旋光仪的观测，我们确定了日冕中等离子体密度的空间分布以及等离子体内主要横向磁流体动力波的相速度。我们结合这些测量结果来绘制全球日冕磁场的天空分量图。日冕中导出的场强（从 1.05 到 1.35 个太阳半径）大多为 1 到 4 高斯。我们的结果证明了成像光谱在日冕磁场诊断中的能力。