Physics of auroral phenomena : proceedings of the 40th annual seminar, Apatity, 13-17 March, 2017 / [ed. board: N. V. Semenova, A. G. Yahnin]. - Апатиты : Издательство Кольского научного центра РАН, 2017. - 143 с. : ил., табл.

Auroral oval and outer electron radiation belt magnetic storm on October 01, 2012, when relativistic electron fluxes are near the same after storm as before storm. Other panels on Fig. 3a show Dst, solar wind velocity, AE and IMF Bz. Electron spectra at the moments indicated on Fig. 3a by vertical lines are shown on Fig. 3b. It is possible to see the increase of flux without change of spectra slope. The simplest explanation of such spectra change is the adiabatic effect. An order of magnitude change of fluxes can mean the local an order of magnitude change of the magnetic field. However, it requires more careful analysis. 4. Conclusions and discussion Auroral oval mapping to the outer part of the ring current change the traditional approaches to the analysis of magnetosphcric activity and clarify many features, which have yet no adequate explanation including the processes leading to outer belt electron acceleration. We try to demonstrate the deep connection of auroral processes and acceleration of relativistic electrons of the outer radiation belt. The appearance of high amplitude electromagnetic fluctuations simultaneously with acceleration of outer belt electrons may be considered as the natural consequence of turbulent processes at the latitudes o f auroral oval during magnetic storms. Decrease of the magnetic field in the region of auroral oval mapping to the equator and great increase of radial transport lead to relativistic electron deceleration and loses during storm main phase. At the same time, storm time substorms produce comparatively fast electron accelerations in this region and provide the seed population for outer belt electrons. The nearest to the equator position of the auroral oval equatorial boundary determines the location of formed after storm outer belt maximum. This may be connected with first auroral arc brightening during substorm expansion phase onset at the equatorial boundary of the auroral oval, as such brightening is connected with sharp increase of the downward electron flux and probable formation of ion beam of ionospheric ions to the magnetosphere. Such beam can form the peak o f plasma pressure decreasing magnetic field in the region of pressure maximum and form a local trap for accelerated electrons. Only first steps in the study of the connection of auroral processes and acceleration of electrons o f the outer belt were made till now and great work is required for the verification of such connections. However, the real progress o f ground based and satellite observations gives the possibility to solve the problem. Acknowledgements. We acknowledge the members of RBSP and THEMIS teams for the use of data. The work is supported by the grant of Russian Foundation for Basic Research No 15-05-04965 the Presidium of the Russian Academy of Sciences (program 7), and Chilean FONDECYT No 1161356 grant and CONICYT PIA Project"Anillo de Investiga-cion en Ciencia у Tecnologia" ACT1405. References Alekseev, 1.1., and V.P. Shabansky (1972), A model of a magnetic field in the geomagnetosphere. Planetary and Space Science 20, 117-133, doi:10.1016 /0032-0633(72)90146-8. Antonova, E.E. (2006) Stability of the magnetospheric plasma pressure distribution and magnetospheric storms. Adv Space Res 38, 1626-1630. doi:10.1016/j.asr.2005.05.005. Antonova, E.E., I.P. Kirpichev, V.V. Vovchenko, M.V. Stepanova, M.O. Riazantseva, M.S. Pulinets, I.L. Ovchinnikov, and S.S. Znatkova (2013), Characteristics of plasma ring, surrounding the Earth at geocentric distances ~7~ 10RE, and magnetospheric current systems, Journal o f Atmospheric and Solar-Terrestrial Physics 99, 85-91, doi:10.1016/j.jastp.2012.08.013. 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