Physics of auroral phenomena : proceedings of the 33rd Annual seminar, Apatity, 02 - 05 March, 2010 / [ed.: A.G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2011. - 206 с. : ил.

О. V. Kozyreva andN.G. Kleimenova pulsations had the same spatial distribution (Fig. 3, interval 3) as during the main phase of this storm (Fig. 3, interval 2), but at a little higher latitudes with the center at ~70°. We suppose that the interval 3 on May 12, 2006 could be applied to the early recovery phase of the CIR-storm. In this time the Pc5 spatial distribution was very similar to the storm main phase one. In the late recovery phase (Fig. 3, interval 4) the Pc5 pulsations were recorded at the polar latitudes both in the CIR- and CME-storms. Thus, a basic difference in the Pc5 geomagnetic pulsations during CIR- and CME-storms is the different wave intensity and the different latitudinal location of the maximum o f the ULF waves activity: in the CIR-storms the Pc5 amplitude is several times lower, and they are observed on the higher latitudes than the CME-storms. 4. Conclusion The analysis o f daytime ULF activity during 10 recurrent storms (CIR- storms) in the minimum of the 23rd solar cycle (2006) showed that high velocity of the solar wind (more than 600 km/s) it contributes to enhancement of the generation ULF waves in the Earth magnetosphere, apparently, due to the development o f Kelvin-Helmholtz instability on the magnetopause. On the earth's surface the most intensive daytime Pc5 geomagnetic pulsations in all phases of CIR-storms were observed predominantly in the pre-noon sector on the latitudes higher than 70°, while in the CME-storms - on the latitudes lower than 70°. A cknow ledg em en ts. This work was supported by Russian Foundation for Basic Research (project no. 10-05-00247) and partially the Presidium of Russian Academy o f Sciences (Program 4). References Borovsky J. E., and Denton М. H. “Differences between CME-driven storms and CIR-driven storms”, J. Geophys. Res., I l l , doi: 10.1029/2005JA011447,2006. Engebretson M. J., Glassmeir K.-H., and Stellmacher M. “The dependence of high-latitude Pc5 power on solar wind velocity and phase of high-speed solar wind streams”, J. Geophys. Res., 103, 26271- 26283, 1998. Kozyreva О. K , Kleimenova N. G., and Schott J.-J. “Geomagnetic Pulsations at the Initial Phase of a Magnetic Storm,” Geomagn. Aeron. 44, 33—41, 2004. Kozyreva О. V., and Kleimenova N. G. “Estimation o f Storm-time Level of Day-Side Wave Geomagnetic Activity Using a New ULF Index,” Geomagn. Aeron. 48, 4 9 1 ^ 9 8 , 2008. Kozyreva О. V., and Kleimenova N. G. “Variations in the ULF Index o f Geomagnetic Pulsations during Strong Magnetic Storms,” Geomagn. Aeron. 49, 425 ^37 ,2009 . Kozyreva O., Pilipenko V., Engebretson М. K , Yumoto K , Waterman J., and Romanova N., “In Search of a New ULF Wave Index: Comparison of Pc5 Power with Dynamics of Geostationary Relativistic Electrons,” Planet. Space Sci., 55, 755- 769, 2007. Mathie R. A., and Mann I. R. “A correlation between extended intervals of ULF wave power and storm­ time geosynchronous relativistic electron flux enhancements”, Geophys. Res. Lett., 27, 3261- 3264,2000. O’Brien T. P., McPherron R. L., Somette D., Reeves G. D., Friedel G. D., and Singer H. H. “Which magnetic storms produce relativistic electrons at geosynchronous orbit?”, J. Geophys. Res., 106, 15533-15544,2001. Singer H. J., Russell С. Т., Kivelson M. G., Greenstadt E. W., and Olson J. V. “Evidence for the control o f Pc 3,4 magnetic pulsations by the solar wind velocity”, Geophys. Res. Lett., 4(9), 377-379,1977. Tsurutani B.T., Gonzalez W. D., Gonzalez A.L.C., Guamieri F.L., Gopalswamy N., Grande М., Kamide Y., Kasahara Y., Lu G., Mann I., McPherron R., Soraas F., and Vasyliunas V. “Corotating solar wind streams and recurrent geomagnetic activity: A review”, J. Geophys. Res., I l l , Doi:10.1029/2005JA011273,2006. Yermolaev Yu.I., and Yermolaev M.Yu., “Statistical Relationships between Solar, Interplanetary, and Geomagnetospheric Disturbances, 1976 - 2000,” Kosm. Issled., 2002, 40(1), 3 - 16,2002. 36