Key points are not available for this paper at this time.
We present detailed extreme ultraviolet (EUV) spectra of four large solar flares: M5.6, X1.3, X3.4, and X17 classes in the spectral ranges 176–207 Å and 280–330 Å. These spectra were obtained by the slitless spectroheliograph SPIRIT onboard the CORONAS-F satellite. To our knowledge, these are the first detailed EUV spectra of large flares obtained with a spectral resolution of ∼0.1 Å. We performed a comprehensive analysis of the obtained spectra and provide identification of the observed spectral lines. The identification was performed based on the calculation of synthetic spectra (the CHIANTI database was used), with simultaneous calculations of the differential emission measure (DEM) and density of the emitting plasma. More than 50 intense lines are present in the spectra that correspond to a temperature range of T = 0.5–16 MK; most of the lines belong to Fe, Ni, Ca, Mg, and Si ions. In all the considered flares, intense hot lines from Ca xvii , Ca xviii , Fe xx , Fe xxii , and Fe xxiv are observed. The calculated DEMs have a peak at T ∼ 10 MK. The densities were determined using Fe xi –Fe xiii lines and averaged 6.5 × 10 9 cm −3 . We also discuss the identification, accuracy, and major discrepancies of the spectral line intensity prediction.
Shestov et al. (2013) studied this question.