Benchmarking atomic data for astrophysics: Fe VIII EUV lines
DAMTP, Centre for Mathematical Sciences, Wilberforce road, Cambridge CB3 0WA, UK e-mail: GDelZanna@spd.aas.org
Accepted: 17 September 2009
The EUV spectrum of 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 3s2 3p5 3d2 4Dj 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.
Key words: line: identification / atomic data / Sun: transition region / techniques: spectroscopic
© ESO, 2009