期刊
ASTRONOMY & ASTROPHYSICS
卷 508, 期 1, 页码 513-524出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/200912557
关键词
line: identification; atomic data; Sun: transition region; techniques: spectroscopic
资金
- STFC (Advanced Fellowship and APAP network)
- STFC [ST/H000429/1, PP/D002907/1, ST/G002584/1, PP/E004857/2, PP/E001254/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/D002907/1, ST/H000429/1, PP/E001254/1, ST/G002584/1, PP/E004857/2] Funding Source: researchfish
The EUV spectrum of Fe VIII is reviewed, using new solar observations from the Hinode EUV Imaging Spectrometer (EIS), together with older solar and laboratory data. The most up-to-date scattering calculations are benchmarked against these experimental data, with the use of a large atomic structure calculation. Once adjustments are made to the excitation rates, good agreement is found between calculated and observed line intensities. All previous line identifications have been re-assessed. Several lines are identified here for the first time, most notably the strong decays from the 3s(2) 3p(5) 3d(2) D-4(j) levels. It is shown that they provide a new, important diagnostic of electron temperature for the upper transition region. The temperatures obtained at the base of solar coronal loops are lower (log T [K] = 5.5) than those predicted by assuming ionization equilibrium (log T [K] = 5.6), however firm measurements will only be possible once better scattering calculations are available, and the EIS radiometric calibration is properly assessed.
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