Solar Coronal Lines in the Visible and Infrared: A Rough Guide
Solar Coronal Lines in the Visible and Infrared: A Rough Guide
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DOI：
10.3847/1538-4357/aa9edf
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发表时间：
2017-08
期刊：
影响因子：
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通讯作者：
G. del Zanna;E. DeLuca
中科院分区：
文献类型：
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作者：
G. del Zanna;E. DeLuca
我们回顾了日冕的可见光和红外线，收集以前的观测数据，并将观测到的辐射与各种模型预测的辐射进行比较：安静的太阳（QS），适度活跃的太阳，以及在边缘附近观察到的活动区域，大约1.1 R。我们还模拟了QS情况下的离边辐射。我们在CHIANTI版本8中使用了最新的原子数据。比较结果是令人满意的，因为所有的强可见线现在都有了明确的标识。我们修正了以前的几个鉴定，并提出了一些新的鉴定。我们还列出了大量我们目前没有原子数据的观察到的谱线，因此仍在等待确定。我们还表明，一个显着数量的日冕线应该是可观察到的光谱的近红外区域由即将到来的丹尼尔K。Inouye太阳望远镜（DKIST）和AIR-Spec仪器，在2017年8月21日日食期间观察日冕。我们还简要讨论了许多潜在的光谱诊断可用于可见光和红外线，特别强调电子密度和化学丰度的测量。我们简要地指出了一些潜在的诊断，可以与未来的红外仪器，正在建造的DKIST和计划的日冕太阳磁场观测。最后，我们强调需要进一步改进原子数据。
We review the coronal visible and infrared lines, collecting previous observations and comparing, whenever available, observed radiances to those predicted by various models: the quiet Sun (QS), a moderately active Sun, and an active region as observed near the limb, around 1.1 R⊙. We also model the off-limb radiances for the QS case. We used the most up-to-date atomic data in CHIANTI version 8. The comparison is satisfactory, in that all of the strong visible lines now have a firm identification. We revise several previous identifications and suggest some new ones. We also list the large number of observed lines for which we do not currently have atomic data, and therefore still await firm identifications. We also show that a significant number of coronal lines should be observable in the near-infrared region of the spectrum by the upcoming Daniel K. Inouye Solar Telescope (DKIST) and the AIR-Spec instrument, which observed the corona during the 2017 August 21 solar eclipse. We also briefly discuss the many potential spectroscopic diagnostics available to the visible and infrared, with particular emphasis on measurements of electron densities and chemical abundances. We briefly point out some of the potential diagnostics that could be available with the future infrared instrumentation that is being built for DKIST and planned for the Coronal Solar Magnetism Observatory. Finally, we highlight the need for further improvements in the atomic data.