Benchmarking atomic data for astrophysics: Fe VII and other cool lines observed by Hinode EIS
Benchmarking atomic data for astrophysics: Fe VII and other cool lines observed by Hinode EIS
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天体物理学原子数据基准：Fe VII 和 Hinode EIS 观测到的其他冷线
DOI：
10.1051/0004-6361/200913082
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发表时间：
2009
影响因子：
6.5
通讯作者：
G. Zanna
中科院分区：
文献类型：
--
作者：
G. Zanna
用新的电子碰撞激发速率、原子结构计算和实验数据，对FeVII的极紫外光谱进行了综述。特别是，使用了从Hinode EUV成像光谱仪(EIS)获得的太阳黑子环谱的太阳观测。以前的品系识别，主要基于实验室的口头数据，已经进行了评估。从3s2 3p5 3D3组态的衰变发现，观测到的谱线强度和波长与预测的有很大的差异，这些谱线是很强的EUV谱线。我们将这些差异归因于不正确的线路标识。提出了一些新的识别方法。在此基础上，发现理论数据与实验数据符合得很好。首次观测到一些跃迁，特别是来自3S23P63D4S组态的跃迁，为测量太阳跃迁区域的电子温度提供了一个新的重要诊断方法。在日冕环底测得的温度接近电离平衡的最大丰度温度(logT[K]=5.4)。对Fevii线的评估是在评估EIS观察到的所有最强冷线的同时进行的。这一光谱在过渡区谱线中非常丰富。提出了一些新的识别方法，特别是Feix的识别方法。大多数最强的转变都已确定，但仍有大量的线等待确定。
The EUV spectrum of Fevii is reviewed, using new rates for electron impact excitation, atomic structure calculations, and experimental data. In particular, solar observations of a Sunspot loop spectrum obtained from the Hinode EUV Imaging Spectrometer (EIS) are used. Previous line identifications, mostly based on lab oratory data, have been assessed. Large discrepancies between observed and predicted line intensities and wavelengths are found for the decays from the 3s 2 3p 5 3d 3 configuration, which are strong EUV lines. We ascribe these discrepancies to incorrect line ide ntifications. A number of new identifications are proposed. W ith these, very good agreement between theory and experimental data is found. A few transitions, in particular from the 3s 2 3p 6 3d 4s configuration, are observed for the first time, and are shown to provide a new important diagnostic for measuring the electron temperature in the solar transition region. The temperatures obtained at t he base of solar coronal loops are found to be close to the temperature of maximum abundance in ionization equilibrium (log T [K]= 5.4). The assessment of the Fevii lines was done in conjunction with an assessment of all the strongest cool lines observed with EIS. This spectrum is rich in transition region lines. Some new identifications are presented, in particular for Feix. Most of the strongest transitions are identified, however a large number of lines still awaits firm identification.