Physics of auroral phenomena : proceedings of the 39th annual seminar, Apatity, 29 February-4 March, 2016 / [ed. board: N. V. Semenova, A. G. Yahnin]. - Апатиты : Издательство Кольского научного центра РАН, 2016. - 167 с. : ил., табл.

I. V. Despirak et al. IT: 17:36:40 17:38:30 17:41:10 17:43:20 17:44:30 17:45:30 17:25 17:36:40 18:00 Figure 2. Development of the substorm on 17 March 2015 in 17:36:40 by chosen all-sky images (top panel), by all­ sky keogram (left bottom panel) and Guppy (GC) camera keograms (right bottom panels). In the GC keogram, the substorm auroras are seen from 17:42:30 UT at the South part of the field of view, at 35° from zenith, due to the fast movement to North. Then a maximal intensity of 200 rel. units was observed about 17:46:25 UT. Case 2: 17 March 2013 Figure 3. Solar wind and IMF parameters and SYM/H index on March 17-18, 2013. The onset times of two substorms are marked by dashed black vertical lines. The solar wind conditions taken from the OMNI database for the magnetic cloud on 17-18 March 2013 are presented in Fig. 3. The time period of the magnetic cloud (MC) (15 UT, 17 March - 6 UT, 18 March 2013) and the region of interaction of MC with the undisturbed solar wind (Sheath) (06-15 UT on 17 March 2013) are marked as red and blue crosshatched areas, respectively. A geomagnetic storm developed during this time. The DST index reached ~ -140 nT. Under these highly disturbed conditions, during the main phase of the storm, two substorms were observed at 18:26 UT and 18:39 UT, 17 March 2013 by the all-sky camera in Apatity. The onset times of these substorms are marked by black dashed vertical lines. 13