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.

L. N. Makarova at al. Long-term variations of the noon values of hmaxF2 demonstrate tendency to increasing from 20 to 21 and 22 cycle and decreasing to 23 cycle (see Fig. 1, middle right panel). 10- 8- Hc 5(/) 6- m 4- l\l\ trl \ ■■ • I я \ щ '■ V \ I \ • 1970 19 8 0 1990 2000 2 8 0 n 2 7 0 - E 260 - X re E 250- <z 240- 230- . . ' 2 '- > A i 1 i ■ ■ * . ■ ■ ■ \ if 150- 1 2 0 - 90- 5 60- 30 0 r= 0 .95 s r ' • • y* • • • %’t Г» « 1970 1980 1990 2000 r= 0 . 8 8 4 5 6 7 fo F 2 , M H Z Figure 1. Long - term (1965 -2007) variations of annually averaged values o f the Sun spot number (W), full vector of the IMF (Bsw), critical frequency (hmaxF2), values o f altitude of maximum o f F2 layer (hmaxF2) on station Sodankyla together with the statistical relations between them. One can see maximum values of Bsw и hmaxF2 during 21 and 22 cycles and minimum during 20 and 23 cycles. The value of the coefficient correlation between Bsw and hmaxF2 is equal 0.88. High value o f the coefficient correlation between of the full vector IMF and altitude of maximum o f F2 layer indicates physical mechanism connection of these parameters. Such physical mechanism can be electric drift of F2 layer under influence of electric field which is connected with IMF. Simulations and experimental data show that electric drift changes o f altitude o f maximum of F2 layer (hmax F2) can be several kilometers for ten minutes. Importance o f distribution o f electric fields in magnetosphere and ionosphere is confirmed by a high value of the coefficient correlation between o f the full vector IMF and altitude of maximum of F2 layer. It means also that value o f the full vector o f the solar wind magnetic field determines character of the electric fields distribution in the near-Earth space. The results o f the recent studies showed that other processes in the near-Earth space besides ionospheric dynamics are closely connected with value of the full vector of the solar wind magnetic field. Analysis o f experimental data showed that both horizontal and vertical components of the IMF averaged annually do not demonstrate any notable deviations from their zero values. Annually averaged values of Bx, By, and Bz components are equal to +/- 0.4 nT. No any periodicity was discovered in variations of these parameters during the period of observations. The solar wind velocity value averaged for the whole period of observations (40 years) turns out to be 444 km s'1. Spectral analysis o f the solar wind velocity data revealed two distinct maximums of power spectra equal to 5 and 10 years. The most definite maximums of the solar wind velocity values were observed in 1974, 1984, 1994, and 2004, i.e. in the years o f minimal solar activity Approximately the same periods of oscillations (5 and 10.8 years) are observed in variations o f the solar wind density. One can find in the long-term variations o f the solar wind density some evidences o f existence of cyclic 80