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.

Solar sources o f intensive geomagnetic storms during the 23rdsolar activity cycle Conclusions 1. During the 23rd solar cycle (1996-2009) as in the previous ones, very intensive storms were observed near the maximum of solar activity and its decay phase. They were caused by CME "halo"-type, accompanied by solar flares and disappearances of filaments. The geoeflective CME were located mainly near the central meridian oi the Sun and had the solar wind velocity over 700 km/s. 2. In addition to the analysis of solar sources for the period 1976-1979 [Joselin, 1986] it was found: a) not only high-class flares, but also weak flares can cause very intensive magnetic storm; b) long living flares play a significant role in the development of geomagnetic disturbances; c) in the period under consideration, phenomenon of disappearance of filaments, unaccompanied flares, rarely (<10% o f storms) led to intensive magnetic disturbances. In solar cycle 23, we found that only 14% of large magnetic storms are related to coronal holes. In the previous cycle, according to [Joselin, 1986] coronal holes preceded 52% o f intensive storms. 3. All the flares and filament’s disappearances, followed by intensive or extreme magnetic storms, were located on the boundaries of sub-sectors (OR-regions) or in the vicinity of the HCS projection. References Hundhausen A.J. Coronal expansion and solar wind. Moscow, Mir, 1986, p. 302 Svalgaard L. Geomagnetic activity: Dependence on solar wind parameters in Coronal Holes and Speed Wind Streams. Colorado Associated University Press, Boulder, Colo., 1977, p. 371 Sheely Ir. N. and Harvey J.W. Coronal holes, solar wind streams, and geomagnetic disturbances during 1978 and 1979. Solar Phys., 1981,70,237. Joselin J. A., McIntosh P.S. Disappearing solar filaments: a useful predictor of magnetic activity. J. Geophys. Res. 1981, V, 86, A6, P. 4555. Joselin J. A. SESC. A Catalog of white light mass ejections observed by SOHO spacecraft. Methods for short - term geomagnetic predictions.-Terr. Predict. Proc. Workshop. Meudon. June 18-22, 1984, Boulder, Colo., Mass. 1986, P. 404. Yahiro S., Gopalswamy N. et. al. A Catalog of white light mass ejections observed by SOHO spacecraft. J. Geophys. Res. 2004, V. 109, doi: 10.1029/2003A010282, P. 105. Webb D.F., Clive E.W et al. Relations of halo coronal mass ejections, magnetic clouds, and magnetic storms. J. Geophys. Res. 2000, V. 106, № A4, P. 7491. Wang Y. М., Wang P.Z., Ye S. et al. A statistical study on the geoeffectiveness of Earth-directed coronal mass ejections from March to December 2000. J. Geophys. Res. 2002, V. 107, (Al 1), doi: 0.1029/2003J2003JA009244. P. SSH Zhao X. P., Webb D. F. Source regions and storm effectiveness of frontside full halo coronal mass ejection. J. Geophys. Res. 2003, V. 108, № A6, doi: 10.1029/2002JA009606, P. 12134. Srivastava N., Venkatakrishnan. P. Solar and interplanetary sources of major geomagnetic storms during 1996-2002. J. Geophys. Res. 2005, V. 110, doi: 10.1029/2005JA011218, A ll 104 Kim R.S., Cho K.-S. et al. Forecast evaluation of the coronal mass ejection (CME) geoeffectiveness using halo CMEs from 1997 to 2003. J. Geophys. Res. 2005, V. 110, doi: 10.1029/2005JA011218. Tsurutani B.T., Gonzalez W. et al. Origin of Intensity Southward Magnetic Fields Responsible for Major Magnetic Storms Near Solar Maximum (1978-1979). J. Geophys. Res. 1988, V. 93, № A8, P. 85191. Lepping R.P., Jones W. D, Burlaga L.F. Magnetic Field of Intensity Magnetic Clouds at 1 AU. J. Geophys. Res 1990, V .95,A8,P. 957. Ivanov K.G., A. F. Kharshiladze Slow Dynamics of Open Field Lines as an Indicator o f Subphotospheric Interactions and Its Relation to Solar Activity Events and Near-Earth Disturbances: 2. Events o f M arch - September. Geomagnetism and Aeronomy, 2002, T. 42, № 2, P. 155. Ivanov K.G., Romashets E., Vandas M. The series of solar-terrestrial extra storms o f May-October 2000. Structure of the bow shock layer and configuration of the near-Earth magnetic cloud on July 15. Geomagnetism and Aeronomy, 2005, 45, N 3, P.315-325. Kharshiladze A. F„ K. G. Ivanov. Spherical harmonic analysis of the solar magnetic field. Geomagnetism and Aeronomy, 1994, 34, N 4, P. 22-32. 22