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.

V.L. Petrov, M.I. Panasyuk After the inter-calibration the long period of time was studied using the data. On the figure 2 (a) one can see 3 curves of the electron flux at L < 1.2. The 0°-channel, Ee > 30 keV is shown at 3 areas as an example. SAA means the border о Southem-Atlantic Anomaly at -800 km altitudinal slice. The difference between the northern and the southern hemispheres is quite low that tells us about the symmetry of the particles loss process. Indeed, the loss of a radiation belt particles is determined by interaction with VLF waves, and this interaction process occurs mainly near the equator. The fluxes in SAA subside to the solar activity cycle minimum, while the fluxes under the belt remain approximately the same level, experiencing variations twice a year. The vertical columns point some o f the important geomagnetic events. The connection between the electron flux increases and high-level geomagnetic activity is beyond doubt. However, the relationship between the electron flux at L < 1.2 and Dst and Kp indexes in quiet geomagnetic conditions have not been found. On fig. 2 (e) it is shown the average rate of GCRs by Moscow neutron monitor station ( http://helios.izmiran.troitsk.ru/cosrav/main.htm and further on the links). The semiannual variations cannot be generated also by the cosmic rays variations. Conclusion There are still many questions about the behavior o f the electrons deep under the radiation belts. The long-term downward trend from 2005 till the end of 2009 is largely coincides with the behavior o f the radiation belts electrons. The decrease in their fluxes can be explained by a small number o f substorms in that period, and as a result, a small number o f incoming particles in the belt. The semiannual variation is to reduce the flux of electrons in the loss cone in summer and winter and increase the number of quasitrapped particles at the same time. This variation appears at L < 2. It is best seen in years 2006 to 2009 when quite geomagnetic conditions gave the least interference in the electron fluxes. The causes of these variations have yet to learn. More information will be get during the increase phase o f the new solar cycle. The work in this direction will continue. References Grigoryan, O.R., Panasyuk, M.I., Petrov, V.L., Sheveleva, V.N., Petrov, A.N. Spectral characteristics o f electron fluxes a t L < 2 under the Radiation Belts. Adv. Space Res., Vol. 42,2008. 1523-1526. Nagata, K., Kohno, Т., Murakami, H., et al. Electron (0.19—3.2 MeV) and proton (0.58-35 MeV) precipitations observed by OHZORA satellite at low latitude zones L = 1.6-1.8. Planet. Space Sci. 36,1988. 591-606. Voss, H.D., Smith, L.G. Global zones o f energetic particle precipitation. J. Atmos. Terr. Phys., Vol. 42, 1980. 227- 239. http://clustl.wdcb.ru/spidr/home.do (SPIDR geophysical data catalogue) http://helios.izmiran.troitsk.ru/cosray/main.htm (Moscow neutron monitor data) http:/fyvww.oso.noaa.gov/poes/index.htm (NOAA POES satellites, instrument description, current status, databases) 146