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.

A.E. Levitin etal. As it is seen in Fig. 5 according to analyzing the DMSP F13 precipitating particle data during the CHAMP passage (at -06.50 UT, and ~ 08.30 UT) the precipitating particle enhancement is seen in the area of the PE development. Fig. 6 shows the CHAMP magnetic field data ( http://op.gfz-potsdam.de/champ) , and auroral oval location according to OVATION model {http://sd_www.jhitapl.edu/Auiora/ovatioii/} for 30 May 2003. It is seen that IMAGE high-latitude sector is located into the dayside auroral oval. 1Л 00(00:00 0в:22Л10835:42 0&2833 08:31:25 0B:34:19 0B:37:07 08:18:59 M aV 3 0 MLAT 0 0 54..1 63.0 70.8 75Л 75.4 69.5 I U 3 GUT 0.0 58.1 67.5 76.2 81.1 76 S 68.4 58.» QL0N0 00 136.1 127.8 109.B 61-5 9.8 360.2 341.3 MIT ООЮО 17:20 16:46 15:42 13(42 11:03 08:17 08:23 ELECTIONS 10 EAC 2 * V/V.>>Av^V■ • - v : ij р.Чь.(j §§ 11 •та*(Я........ . L :j:;"> Ж'1 . ПТПТr v:jvМ И Ш Щ ШШ & 03/150 LOG E FLUX ELEC ION 101 UT 0000:00 OCHXcOO 06:41:25 06:47:06 0&52JC 06:58:33 00:00:00 00d0:00 Mt>T 0.0 0Л 38.7 71.8 72-9 36.9 0.0 0.0 (ХАТ 00 0J> 98.5 77.4 75Л 57.3 0.0 0.0 olono oo OlO ieo.7 1зав 31.1 ъ л o.o о о MIT ООЮО 00:00 16:58 14:57 10:11 07Л9 00Л0 OCkOO s L May 30 Figure 5. The DMSP F13 precipitating particle data during the CHAMP passage: (top) 06.50 UT, (upper) 08.30 UT. The geomagnetic pulsations and solar wind and IMF fluctuations have been studied by applying a new approach to data processing based on fuzzy logic methods of discrete mathematical analysis (DMA) [Zelinsky et al„ 2014]. Fig. 7 and Fig. 8, the wave structure of considered day- side magnetic bays was represented by the 2-7 mHz geomagnetic pulsations which do not observed in the solar wind and IMF, and demonstrated the spectral properties different from the resonant Pc5 waves. The direct penetration of fluctuating solar wind electric fields in the polar cap was of low probability, since the bursts of geomagnetic pulsations on the Earth’s surface and IMF parameters fluctuations were incoherent. Final conclusion about a physical mechanism of excitation of the daytime polar substorm (PE events) and accompanying geomagnetic pulsations requires further detailed experimental and theoretical studies. Summary 1. We presented two events of the polar electrojet (PE), i.e. dayside polar latitude magnetic bay, which sign is controlled by the IMF By. 2. We found that the PE development is the magnetosphere respond to the high positive values of the IMF Bz occurrence during the magnetic storms. 3. The PE were observed at the same polar region where the NBZ system of the field aligned current (FAC) may be enhanced (according the IZMIRAN model [Feldstein and Levitin, 1986]). The sequences of two geomagnetic vortices with opposing rotation directions (upward and downward FAC) observed during the second event and one vortex with the clockwise rotation in the first one support this proposal as well as the CHAMP spacecraft data. 4. The dayside polar magnetic bays (PE) were accompanied by the (2-7) mHz geomagnetic pulsations with the spectral properties different from the resonant Pc5 waves. ^ Мурманская государственная областная универсальная научная библиотека 17 CAP fVIПг.--.4'.1л>'Mi i <irvO N: W - JcWt'iu tj:; !.< 11'i Figure 6. The CHAMP magnetic field data and the auroral oval location (OVATION).