Speaker
Description
Hinode EIS observations of flares are used to discuss the potential diagnostics
of hot (5-15 MK) plasma for the short wavelength channel of EUVST.
Several lines, rarely or never observed previously, are reported.
Comparisons between theoretical and observed intensities is generally very good, using my recent EIS radiometric calibration. However, discrepancies are present for a few cases, indicating the need for new atomic calculations.
A new programme for laboratory astrophysics is presented. Electron Beam Ion Trap spectra will finally observe several EUV flare lines predicted to be visible but never observed. Also, detail analysis will help resolving the identifications of the forest of coronal lines that are blending the flare lines in the soft X-rays such as the Fe XIX line, the main target of MUSE.
