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.

On solar cosmic raypropagation in the interplanetary space and highly ionized ions emission which occurred in the center of the disk and recorded on the Earth's orbit, is delayed almost 10 hours. That occurred for all flares that appeared in the center of the disk or its eastern part. The gentle front o f proton flux order o f a day is a typical for such a flare. These protons can propagate to GOES across the magnetic field lines due to diffusion. The flare on the limb o f the solar disk makes it possible to observe energy accumulation and energy release in the corona outside the disk, when the contribution of the luminescence of the solar disk is completely eliminated. The flare that very convenient for observation has been appeared in July 23, 2002 [8], when it is clearly shown that the source of the thermal X-ray emission from the X4.8 flare is a plasma cloud in the corona The number o f particles is ~ 1037. Despite this fundamental result o f Lin et al., several recent Russian papers have appeared [9], which state that the flare is a typical chromospheric phenomenon. Unfortunately, for the 2002 flares there are no photographs in various UV spectral lines that can demonstrate the pre-flare state in different plasma temperatures. Figure 2. Pre-flare condition and flare X I.6 in the coronal line 94 A according to SDO. The right panel shows the thermal X-ray radiation and solar cosmic rays according to GOES. Figure 3. Pre-flare condition and flare on the East limb in the emissions from cold plasma of the chromosphere and the hot plasma o f the solar corona. Fig. 3 shows several frames taken from the archive of the SDO AIA spacecraft, which demonstrate the emission of various pre-flare spectral lines of the XI.4 flare observed on the eastern limb. Such rare phenomenon has been accompanied by the cosmic radiation with the delay of ~ 20 h, since the GOES devices could detect protons from such flares only after their drift across the magnetic field lines. The top photos of Fig. 3 demonstrate emission of the rather cold line of Hel on the eastern limb observed the half hour before the flare. May be, the Hel emission is appeared much earlier on the back side of the Sun, but it became clearly visible only after 09:00 as a result of Sun rotation. Before the flare a noticeable change in the structure of Hel emissions is not observed, and during the flare only a slight heating of the chromosphere is seen. The coronal line 94 emission slowly increases over the Sun surface in the phase of energy accumulation. It also increases during the flare. The other behaves demonstrate the emission of lines of ПРЕДВСПЫШЕЧНОЕ СОСТОЯНИЕ И ВСПЫШКА SDOAiA AR1215S N11E05 0Э4А Fe XVill 10 September 2014 10=17:21 X1.6 9:43:38 15:45:0; 16:44:14 16:59:38 17:15:02 17:29:14 17:44:40 17:59:14 22.09.2011. X1.4 AR11302 t 0= 10:30 Hei 50000K Э4А FeXVHI 6 .3M K 193A F e X X X tV 2 0M K 80