Physics of auroral phenomena : proceedings of the 34th Annual seminar, Apatity, 01 - 04 March, 2011 / [ed.: A. G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2011. - 231 с. : ил.

L.L. Lazutin, T.V. Kozelova increased gradually, indicating on the radial diffusion process. Similar effect of the moderate radial diffusion was registered on 1.7 MeV electron channel. Discussion An enhancement of the relativistic electron flux in the inner magnetosphere including the slot region (L = 2 - 3), was frequently observed at the beginning of storms [e.g., Baker et al., 1994, 2004; Li et al., 1997; Kanekal et al., 2001]. The flux increase is observed by low- altitude spacecraft are not caused simply by an enhanced precipitation rate because it was registered near the equatorial plane as well [Baker et al., 1994]. Time scale of the flux increase ws too short for the acceleration by radial diffusion caused by the resonance with ULF-Pc5 magnetic pulsations . This type of the acceleration is widely discussed [see review by Spritz et al., 2008]. Fast injection by SC also must by excluded from the discussion, therefore substorm associated injections remains as a best candidate. From the substorm case studies it is known that ExB radial injection during local magnetic field dipolarization is the main source of the energetic auroral electron acceleration up to 300 keV measured by balloons bremstrahlung auroral X-ray bursts [Lazutin, 1986 and references therein]. During one year of the SERVIS-1 observations we found 6 cases of the fast electron flux increases coinciding with substorm activations. That is the main finding of the present study: close relation of the fast electron injections with auroral activations. In all cases fast increases were observed in a channel 0.3-1.7 MeV and in three case less intensive increases were registered in a channel >1.7 MeV. That outlines the upper energy limit of the fast radial injection effect approximetely near or less than 1 MeV. Time scale of the intensity increase was between 0.5 and 1.5 hours. There may be two possible scenarios how auroral activation creates observed fast electron increases. It can be direct injection of the auroral electrons during the process of the substorm acceleration. It is known that during magnetic storm auroral activity region is shifted toward lower latitudes following the radial displacement of the radiation belt. Another model may be proposed when “old” radiation belt electrons are accelerated by the pulses propagated inward from the substorm activation region. The mechanism is similar to the fast injection by SC pulse and can transport electrons down to the slot region. Acknowlegements. Authors are gratefull for the magnetometrs data to the colleagues from Jakutsk Institute of the Space Physics Research and Aaeronomie. The work is partly supported by the Programme № VI. 15 of the Division of Physical Sciences of RAS “Plasma Processes in Solar System”. References Baker, D. N., J. B. Blake, L. B. Callis, J. R. Cummings, D. Hovestadt, S. Kanekal, B. Klecker, R. A. Mewaldt, and R. D. Zwickl (1994), Relativistic electron accele­ ration and decay timescales in the inner and outer radia-tion belts: SAMPEX, Geophys. Res. Lett., 21, 409-412. Baker, D. N., S. G. Kanekal, X. Li, S. P. Monk, J. Goldstein, and J. L. Burch (2004), An extreme distortion of the Van Allen belt arising from the “ Halloween” solar storm in 2003, Nature, 432, 878 - 881. Kanekal, S. G., D. N. Baker, and J. B. Blake (2001), Multisatellite mea surements of relativistic electrons: Global coherence, J. Geophys. Res., 106, 29,721 - ,732. Lazutin, L.L. (1986). X-ray emission of auroral electrons and magnetospheric dynamics. Springer- Verlag, Berlin-Heidelberg,./ Physics and Chemistry in Space v.14 /. Li, X., Roth I., Temerin М., Wygant J.R.,.Hudson M.K, and Blake J.B. (1993), Simulations of the prompt energization and transport of radiation belt particles during the March 24, 1991 SSC, Geophys. Res. Lett. 20, 2423. Li, X., D. N. Baker, M. Temerin, Т. E. Cayton, E. G. D. Reeves, R. A. Christensen, J. B. Blake, M. D. Looper, R. Nakamura, and S. G. Kanekal (1997), Multisatellite observations of the outer zone electron variation during the November 3 - 4, 1993, magnetic storm, J. Geophys. Res., 702,14,123-14,140. Nagai, Т., A. S. Yukimatu, A. Matsuoka, К. T. Asai, J. C. Green, T. G. Onsager, and H. J. Singer (2006), Timescales of relativistic electron enhancements in the slot region, J. Geophys. Res., I l l , A11205, doi:10.1029/2006JA011837 Timescales of relativistic electron enhancements in the slot region, J. Geophys. Res., 111, Al 1205, doi:10.1029/2006JA011837 Shpritz, Y.Y., Elkington, S., Meredith, N.P., Subbotin, D.A (2008), Review of modeling of losses and sources of relativistic electrons in the outer radiation belt I:— radial transport, J. Atmos. Solar- Terr. Phys. 70, 1679-1693. Fassiliadis D., Fung S. F., and Klimas A. J. Solar, interplanetary, and magnetospheric parameters for the radiation belt energetic electron flux // J. Geophys. Res. V. 110. A04201. doi: 10.1029/2004JАО10443. 2005. 20