Physics of auroral phenomena : proceedings of the 36th Annual seminar, Apatity, 26 February – 01 March, 2013 / [ed. board: A. G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2013. - 215 с. : ил., табл.

О.I. Yagodkina and V.G. Vorobjev After the shock a velocity grew up from about 450 to 600 km/s, a density increased from 2 to 10 cm'3. The value o f the Dst index in the main phase o f the storm was -42 nT. During the cloud passage the Dst index stayed at about -30 nT and AL index indicated series of substorms. a b 08:00 UT 10:10 UT 16:00UT 4 AL* - 56nT 5 AL= - 853 nT О AL= - 1349nT Dst= - 1&iT Dst= - 23iT Dst= - 22iT Fig. 2 Global distribution of electron precipitation (geomagnetic latitude - local geomagnetic time coordinates) and magnetic activity on Dec. 11 (a) and on Dec. 12 (Z>) In Fig.s 2 global distribution of electron precipitation in corrected geomagnetic coordinates from АРМ and magnetic activity (AL and SYMH indices) on Dec. 11 (a) and on Dec. 12 ( b ) are shown. The global precipitations were constructed according АРМ by using Dst and 5-min AL indices. The locations of the BAB and LOZ stations are marked by points. At the top of each pattern the magnetic activity and UT are shown. The numbers o f vertical dashed lines on magnetic activity curves correspond to the time at which the precipitation patterns were calculated. According to АРМ the BAB and LOZ observatories on Dec. 11 pass through different MLT sectors and zones. BAB located in the polar cap or at the poleward of SDP, and the LOZ placed in DAZ and AOP regions. At the time of SSC (1400 UT, pattern 1) we can see the typical noon-midnight form of auroral precipitation. Before of main phase of storm (1730 UT - pattern 2) the all precipitation zones shifted to pole, and during main phase (pattern 3) the equatorward expansion o f precipitation zones was observed. In the nighttime sector the equatorward boundaries o f the precipitation have shifted to lower latitudes, whereas the position of the poleward boundary depends weakly on the magnetic activity level. This effect was illustrated early by Vorobjev and Yagodkina (2007a). The pattern 3 (2100 UT) demonstrates the small asymmetry of auroral precipitation which typical for the auroral precipitation during the magnetic storms associated with the magnetic clouds ( Yagodkina et al., 2012 ). Dynamic of auroral precipitation and magnetic activity variations on Dec. 12 are shown in Fig. 2b. During this period the series of substorms with typical AL distribution at long-lasting, steady depression of Dst were registered. Power o f substorms increased sporadic. During |AL|- maximum the BAB station was located in the polar cap, and all boundaries have shifted to lower latitudes, the zones o f precipitations expanded. During the expansion phases the typical noon-midnight distribution o f auroral precipitation is observed. Before substorm growth and past of the recovery phases BAB was situated at the poleward edge of SDP. The LOZ station was situated in DAZ or AOP periodically. December11,2004 December12.2004 Fig. 3 The auroral luminosity registered by MSPs at BAB in 630.0 nm (the first panel) and at LOZ in 557.7 nm emissions (the second panel), the location of AOP and DAZ boundaries (white lines inside of the MSP records), AL- and SYM/H indices Fig. 3 displays the auroral luminosities registered by MSPs at BAB in 630.0 nm (the first panel) and at LOZ in 557.7 nm emissions (the second panel), the location of AOP and DAZ boundaries (white lines inside o f the MSP records), AL and SYM/H indices. The meridian scanning photometer at BAB registered aurora on Dec. 12 only. Along the vertical axis at the left panels the elevation angles of 0° and 180° correspond to the southern and northern horizon, respectively. From the right o f panels the boundary 2 2