论文标题
活性区域磁场的Hinode/EIS测量
Hinode/EIS measurements of active region magnetic fields
论文作者
论文摘要
目前的工作说明了一种新的诊断技术的潜力，该技术允许使用少数明亮的\ ion [fe x]和\ ion [fe xi]线的冠状磁场强度测量冠状磁场强度。 The importance of this new diagnostic technique lies in two basic facts: 1) the coronal magnetic field is probably the most important quantity in coronal physics, as it is at the heart of the processes regulating Space Weather and the properties of the solar corona, and 2) this technique can be applied to the existing EIS archive spanning from 2007 to 2020, including more than one full solar cycle and covering a large number of active regions, flares, and even冠状质量弹出。这种新的诊断技术为一个全新的研究领域打开了大门，补充了即将到来的DKIST和UCOMP地面观测站的磁场测量值，并将我们的覆盖范围扩展到在磁盘上观察到的活动区域，直到现在仅通过无线电测量进行采样。在这项工作中，我们介绍了该技术在EIS任务期间在不同时间进行的EIS观察中应用的一些示例，讨论其当前局限性以及提高其准确性的步骤。我们还提供了EIS观察序列的列表，其数据包括应用此诊断技术所需的所有线路，以帮助太阳能社区导航巨大的EIS数据集并找到适合测量冠状磁场的观测值。
The present work illustrates the potential of a new diagnostic technique that allows the measurement of the coronal magnetic field strength in solar active regions utilizing a handful of bright \ion[Fe x] and \ion[Fe xi] lines commonly observed by the Hinode/EIS high-resolution spectrometer. The importance of this new diagnostic technique lies in two basic facts: 1) the coronal magnetic field is probably the most important quantity in coronal physics, as it is at the heart of the processes regulating Space Weather and the properties of the solar corona, and 2) this technique can be applied to the existing EIS archive spanning from 2007 to 2020, including more than one full solar cycle and covering a large number of active regions, flares, and even coronal mass ejections. This new diagnostic technique opens the door to a whole new field of studies, complementing the magnetic field measurements from the upcoming DKIST and UCoMP ground based observatories, and extending our reach to active regions observed on the disk and until now only sampled by radio measurements. In this work we present a few examples of the application of this technique to EIS observations taken at different times during the EIS mission, discuss its current limitations and the steps to improve its accuracy. We also present a list of EIS observing sequences whose data include all the lines necessary for the application of this diagnostic technique, to help the solar community navigate the immense set of EIS data and to find observations suitable to measure the coronal magnetic field.
