Physics of auroral phenomena : proceedings of the 40th annual seminar, Apatity, 13-17 March, 2017 / [ed. board: N. V. Semenova, A. G. Yahnin]. - Апатиты : Издательство Кольского научного центра РАН, 2017. - 143 с. : ил., табл.

I.M. Podgomy and A.I. Podgomy X-ray emissions in the corona during the X4.8 flare in 2002 year above the Eastern limb of the solar disk [8]. These processes should be investigated by UV spectral lines emission of the high ionized iron ions, which are characteristic for the temperature of the solar corona. But such data were not then available. Now the photos of flares and pre-flares state are obtained in the highly ionized iron spectral lines. This information is contained in the data of the SDO archive unit ( sdo.gsfc.nasa.gov ). The most convenient for the analysis of flares are short UV spectral lines 94 A, 131 A, and 193 A. The first of them belongs to ion FeXVIII, and the other to ions FeXXIII and FeXXIV. The maximum of 94A line brightness corresponds to the temperature of 6.3 MK. The emission of 131 A corresponds to 16 MK, and the emission of the line 193 A includes radiation of FeXXIV ions of very hot plasma (20 MK). The phenomena occurred in the chromosphere, where the temperature is low, could not produce hot plasma structures with ions FeXII, XVIII, XXIII, and FeXXIV at energy accumulation in the pre-flare state. Appearance of hot spectral lines demonstrates existence of the phenomena that occurred in the corona. SDGAIA AR12158 September 10 2014 t =17:25 X1.6 94 A Fe XVfi! (6.3 MK) 09'34'32 15:45:02 16:59:38 17:15*02 17 29 14 17:44:40 131 A FeXXIt! (16 MK) 09:26:34 15:42 46 16:41:58 17 12 46 17:28:12 17:42:46 1S3A FeXXIV (20MK) Figure 1. Photos of pre-flare and flare development taken with different spectral lines corresponding to different temperature. The flare is appeared in the solar flare disk (N11E05). The Fig. 1 shows the active region A012158 photos taken with the SDO spacecraft ( sdo.gsfc.nasa.gov ) in spectral lines 94 A, 131 A, and 193 A of highly ionized iron atoms. The photos show the pre-flare state in the corona above the active region and the flare X I.6 that emerged at 17:21 near the center of the solar disk. This flare is accompanied by the generation o f solar cosmic rays. The local emission of the pre-flare UV structure is especially strong before the flare appearing in the line 94 A associated with the temperature 6.3 MK. The shape of the pre-flare structure does not correspond to the shape of the magnetic field lines, which is clearly seen in the photographs. Some of these field aligned emission have an ark shape, but they do not connect with flare appearance. The temperature of the local pre-flare structure is much higher than the chromosphere temperature. So, the pre­ flare process is developed in the corona above an active region, but not in the chromosphere. The flare produces very strong and sharp increasing o f the 193 A spectral line that corresponding to the highest temperatures, but the most strong pre-flare image is demonstrated by the spectral line 94 A. The maxima luminosity o f the 94 A line is achieved at the temperature 6.3 MK. In the place of the pre-flare structure, existed before the flare, the emissions of spectral lines 131 A and 193 A are manifested not strong flare emission, but they demonstrate explosive emission increasing after 17:21. The local strong plasma heating in the corona during the flare is manifested by the appearance of bright emission of spectral lines corresponding to the high temperature T ~ 20 MK. The brightest image during the flare shows the hottest line 193 A. The dynamics of pre-flare and flare emission in the spectral line 94 A are shown in Fig. 2 in details in the larger time interval. From the panels placed in the right side of Fig. 2 it follows that arrival of the proton front from the flare, 79