Physics of auroral phenomena : proceedings of the 38th annual seminar, Apatity, 2-6 march, 2015 / [ed. board: A. G. Yahnin, N. V. Semenova]. - Апатиты : Издательство Кольского научного центра РАН, 2015. - 189 с. : ил., табл.

Influence ojslope o fthe solar wind inhomogeneityfront on properties o f longperiodpulsations during SSC R e ); and to <p = 88° at the orbit of the THEMIS satellites (XGSE» 42 RE) (see. Fig. 4). The arrival of the inhomogeneity front has caused a sharp displacement toward the Earth of the magnetopause nose (its subsolar point) [Shue et al. 1998] before Ssc it was at x= 10.3 RE from the Earth, and after the impact - at the x = 6.7 RE. 18 .00 18.05 18.10 18.15 18.J0 18.25 18-30 18 .00 18.05 18.10 18.15 1SJ0 18.25 18J0 a) fix, nT b) 14.07.2012 BLC 11.25 MLT ' SIT 8.11 MLT Figure 2. The Bx- component variations from data of: a) high-latitude parallels (Ф = 72° and Ф = 67° - 69°) - ground-based observatories of the CANMOS and CARISMA Canadian networks; b) the mid-latitude parallels (Ф = 56° - 59° and Ф = 52° - 54°) - of the CANMOS, CARISMA networks and US ground observatories; c) the low- latitude parallel of US and Japan ground stations. Black arrows show the propagation direction of geomagnetic pulsations. Dotted oval denotes the alleged area of divergence (running away) of geomagnetic pulsations. Fig. 2 shows the results of our analysis of the long- period geomagnetic pulsations propagation at the high, middle and low latitudes in the azimuthal direction. Absolute value of the Bx component of geomagnetic pulsations is shown in Fig. 2a. At the high-parallel Ф = 72° (above the projection of the magnetopause) near noon irregular pulsations move from station BLC (11.25 MLT, A = 190 nT) to IQA (14.00 MLT, A = 70 nT) with a velocity of 14 km/s (Figure 2a). At the parallel Ф = 67° - 69° (right within the magnetopause projection) pulsations propagate from FSMI (9.58 MLT, A = 62 nT) to the morning station DAWS (7.37 MLT, A = 144 nT) at a speed of 50 km/s, and from FCC (11.31 MLT) to the neamoon station GILL (11.34 MLT, A = 108 NT) at a speed of 6 km/s. Fig. 2a shows highlighted oval area of divergence pulsations, which is located between the stations FSMI and FCC. At the parallel Ф = 56° - 59° (close to the projection of the contact area of the front with daytime magnetopause) pulsations propagate from PINA (11.32 MLT, A = 32 nT). After the 3 seconds they were observed at the station WEYB (10.52 MLT), then through 4 s at stations VULC (9.50 MLT, A = 45 nT) and VIC (9.25 MLT, A = 28 nT), and by 33 s - at the morning station SIT (8.11 MLT) (Fig. 2b, upper panel). At the midlatitude parallel Ф = 52° - 54° (Fig. 2b, bottom panel) pulsations run from POLS (9.55 MLT, A = 32 nT) to dawn (SHU, 6.40 MLT) at a speed of 100 km/s, and to dusk (ANNA, 12.32 MLT, A = 20 nT) at a speed of70 km/s, and then to STJ (15.10 MLT, A = 22 nT). At low latitudes (Ф = 15° - 28°, Fig. 2c) pulsations in the afternoon sector propagate duskward from SJG (13.48 MLT, A = 1 nT) to KOU (14.42 MLT, A = 3.5 nT) and further to MBO (17.13 MLT). On the dawn side waves propagated from HON (7.23 MLT, A = 0.8 nT) nightward to КАК (2.46 MLT) at a speed of 140 km/s. Pulsations with a stable polarization were observed for 3.5 - 4 min. Fig. 3 shows the behavior o f the polarization at the high, middle and low latitudes in the dawn, pre- and afternoon MLT sectors (dotted circle with the up arrow - the counterclockwise direction of the polarization vector, the solid circle with the down 12