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 andA.I. Podgomy highly ionized iron FeXXIII and FeXXIV of hot plasma with the temperature of 16 MK and 20 MK, much higher than the normal temperature of the corona. The image in the line 193 is barely visible before the flare, but during the flare a bright image in the corona over o f the solar disk is appeared. The flare energy release is occurred in the corona above the active region. There remains no doubt in the coronal origin of the flare. Fig. 4 shows M5 flare development of on the western limb in the line 193 A. At frame 02:00:20 one can clearly see the appearance of the hot plasma cloud of the flare in the solar corona outside the solar disk boundary. The picture clearly indicates that the flare energy release takes part in the solar corona (black arrow). The pre-flare emission can be seen in all pictures, but the emission is very weak in the hot 193 A line as usual. The flare is accompanied by the flow of solar cosmic rays with a sharp front, arrived with a delay relative to the flare front not more than 20 min. This means that the proton flow front arrive the GOES along the magnetic field lines of the Archimedes spiral without collision. The delay 15 - 20 min is typical for protons arriving from the western flares. PREFLARE STRUCTURES M5 N12W91 AR11476 17 05.2012 !„-0!;2S 593 A FeXXIV 20 MK Figure 4. Pre-flare condition and the M5 flare on the western limb (black arrow) in 193A spectral line from SDO data. The graphs show the flare thermal X-ray radiation and solar cosmic rays according to GOES data. Conclusions The appearance of local sources of UV emission in the corona above an active region before the flare and during the flare is investigated. The data of the SDO spacecraft are used. The pre-flare UV spectral line emission in the corona appears about 2 days. The flare appearance can be predicted by observation o f a high-temperature plasma structure with the length ~10'° cm. The characteristic UV emission can be used for solar flare prognosis. The brightness of the UV emission sharply (~20 min) increases during the flare. The plasma structure above active regions reaches the temperature ~20 MK during the flare. At the solar flare a sharp (several minutes) increasing of the UV spectral lines emission of ions FeXXIV and FeXXIII, localized above the Sun surface, is observed. The strong local heating of the coronal plasma above an active region cannot be explained by the flare energy release on the surface of the Sun in the chromosphere. The flare energy release takes place in the corona. Flare development in the cromosphere is completely excluded. The temperature o f the chromosphere at this time increases very weakly. The rapid arrival o f protons and the steep front of the proton flow from the western flare are created due to the particle propagation along the magnetic field lines of the Archimedes spiral without collisions. The delayed about 10 hours flow o f protons from the eastern flare has a gently sloping front. Solar cosmic rays from the eastern flares can propagate diffusing across the magnetic field. References 1. Podgomy A.I. and Podgomy I.M., Sol. Phys. 139 , 125-145 (1992). 2. Podgomy A.I., Podgomy, I.M.: Astronomy Reports. 50 , 842 (2006). 3. Balabin Yu.V., Vashenyuk E.V., Mingalev O.V., Podgomy A.I. Podgomy I.M. Astronomy Reports. 49, 837 (2005). 4. Podgomy I.M., Balabin Yu.V., Podgomy A.I., Vashenyuk E.V. JASTP. 72, 988 (2010). 5. Podgomy A.I., Podgomy I.M. Astronomy Reports. 59 , 888 (2015). 6. Podgomy A.I., Podgomy I.M. Astronomy Reports. 55 , 629 (2011). 7. Podgomy I.M., Podgomy A.I., Meshalkina N. S. Astronomy Reports. 59 , 795 (2015). 8. Lin R.P., Krucker S., Hurford, G.J. et al. Astrophys. J. 595 , L69 (2003). 9. Stepanov A.V., Zaitsev V.V., Melnikov V.F. et al. (In Russion). Solar solar-Earth physics-2011. Pulkovo. P. 197. 81