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.

A.E. Levitin atal. pressure В2/2ц0 calculating according to paraboloidal model of the magnetoshperic magnetic field [Feldstein et al., 2005] gives good agreement with analytic model results. But it would be preferable to choose PM-use-procedure during magnetic storms when the southern IMF component Bz becomes rather strong (-30 nT < Bz < -20 nT). Table 2. R0 (Re) predicted according to different models for events when geostationary satellite was located close to the magnetopause.________________________________________________________________________ Date Bz, nT N, cm'3 Dp, nPa Ro, Re R n, Re R 0, Re Shue et al. Shue et al. Kuznetsov et [1997] [19981 a l., [1998] Ro, Re PM-used 21.02.79 2.2 22.8 10.74 7.98 7.99 7.71 7.92 25.07.81 -27.0 21.8 21.87 4.77 5.60 4.79 6.23 11.11.83 2.6 12.6 6.11 8.71 8.71 8.58 8.55 12.06.91 17.6 22.2 27.29 6.97 6.97 6.46 6.65 21.02.92 -9.4 17.4 5.94 7.58 7.58 6.78 8.29 Table 3. R 0 RAN. (Re) predicted according to different models for events that have been examined by team of IKI Date Bz, nT N, cm'3 Dp, nPa Ro, Re R 0, Re Shue et al. Shue et al. [1997] [1998] R 0, Re Kuznetsov et al. R 0 , Re PM-used Ro, Re IKI 07.06.81 - 1 1 . 0 34.0 14.40 6.58 6.41 6.45 7.19 6.4 25.07.81 -15.3 10.0 10.90 6.45 6.34 6.82 7.04 6.6 24.05.83 -15.1 15.0 13.31 6.16 6.16 6.16 6.88 6.5 11.12.83 -5.0 7.0 2.95 9.25 9.25 9.32 9.24 6.4 Note that reliable comparison model R0 with satellite measurements could not realizable as a satellites cross the magnetopause in the solar point during a magnetospheric disturbance very rarely. Besides, the magnetopause stand­ off distance R0 should not be estimated rather accurately due to permanent moving of the magnetopause. A c kn ow ledgm en ts. This study is supported by RFBR grants 08-05-00896. References Fairfield, D.N., Average and unusial locations o f the Eath’s magnetopause and bow shock, , J. Geophys. Res., 76, 6700, 1971. Feldstein, Y. I., Levitin, A.E.; Kozyra, J. U., et al., Self-consistent modeling o f the large-scale distortions in the geomagnetic field during the 24-27 September 1998 major magnetic storm, J. Geophys. Res., 110, Al l , A11214 10.1029/2004JAO 10584, 2005. Kuznetsov, S.N., and A.V. Suvorova, An empirical model o f the magnetopause for broad ranges o f solar wind pressure and Bz IMF, in Polar Cap Boundary Phenomena, edited by J. Moen et al., Kluwer Acad., Norwell Mass., 51, 1998. Petrinec, S. М., and С. T Russell, Factors which control the size of the magnetosphere, in Solar Terrestrial Predictions IV, vol. 2, edited by J. Hruska et al., pp. 627-635, Natl. Oceanic and Atmos. Admin. Environ. Res. Lab., Bolder, Colo., 1993. Petrinec, S. М., and С. T Russell, Near-Earth Magnetotail shape and size as determined from magnetopause flaring angle, J. Geophys. Res., 101,137-152,1996. Petrinec, S. М., Song, P., and С. T Russell,., Solar cycle variations in the size and shape of the magnetopause, J. Geophys. Res., 96, 7893, 1991. Roelof, E. C., and D. G. Sibeck, Magnetopause shape as a bivariate function o f interplanetary magnetic field Bz and solar wind dynamic pressure, J. Geophys. Res., 98, 21421, 1993. Sibeck, D. G., Lopez, R. E., and Roelof, E. C.: Solar wind control o f the magnetopause shape, location, and motion, J. Geophys. Res., 96, 5489, 1991. Shue, J.-H, J. K. Chao, H. C. Fu, et al, A new functional form to study the solar wind control of the magnetopauses ize and shape, J. Geophys. Res., 102, 9497, 1997. Shue, J ,-H., et al., Magnetopause location under extremes solar wind conditions, J. Geophys. Res 103 17 691 1998. Sotirelis, Т., and Meng, С-I, Magnetophause from pressure balance,/. Geophys. Res., 104, 6889,1999. 66