Physics of auroral phenomena : proceedings of the 35th Annual seminar, Apatity, 28 Februaru – 02 March, 2012 / [ed. board: A. G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2012. - 187 с. : ил., табл.

O.I. Yagodkina, V.G. Vorobjev The maximum value of electron energy occurs in pre-noon (09-12) and slowly falls down to the evening (18-21). The peak of proton energy is situated in the after-noon (15-18) and its value varies from about 12 keV to 18 keV with the magnetic activity grow. Thus, the maximum proton energy concentrates in the afternoon and pre-midnight sectors in the DAZ, at the equatorial edge of the auroral oval. We compared the proton precipitation from DMSP F6, F7 and F9 spacecraft data and those obtained by means of the empirical formulas for two magnetic storms on February 8-9, 1986 (18-21, 21-24 MLTs), and March 13-14, 1989 (21-24 MLT), with a Dst value at a maximum of approximately -300 and -600 nT, respectively. The energy proton input (average flux and energy) within the DAZ (bli - b2i) and AOP (b2i - b4s, b4s - b5i) was estimated from the model regression equations and compared with DMSP spacecraft data. The scatter in the DMSP data was very large in the DAZ region and reduced in the poleward part of the AOP. The empirical formulas give the close approximation in the poleward part of the AOP. Under large scatter of the experimental data the model regression equations allow to obtain information about the energy input of proton precipitation. The model describes well enough the global distribution of the auroral proton precipitation during the magnetic storms of different intensity and the model calculations are capable of filling the gaps in spacecraft measurements. Conclusion Early obtained the database from the DMSP F6 and DMSP F7 spacecraft data was used to examine the proton precipitation in all sectors of local geomagnetic time. While electrons are the dominant particle energy source in the auroral precipitation, proton precipitation inputs a considerable part in the afternoon and pre-midnight sectors. The maximum proton precipitation was found in DAZ equatorward of the auroral oval. The enhancement o f the proton fluxes and energies is registered with the increasing magnetic activity. The proton precipitation exceeds the electron precipitation during the disturbed conditions. The comparison of the calculated and the experimental data during two magnetic storms illustrates that model calculations could be used for filling gaps in spacecraft measurements especially during large magnetic storms when the spacecraft data are no available. Acknowledgement. This work was supported by RFBR grant 12-05 -00273a and Programs 4 and 22 of the RAS Presidium. References Akasofu, S-I.: Discrete, continuous and diffuse auroras, Plannet. Space. Sci., 22, 1723,1974. Basu, B., J.R. Jasperse, R.M. Robinson, R.R. Vondrak, and D.S. Evans, Linear transport theory of auroral proton precipitations comparison with observations, J. Geophys. Res., 92, 5920, 1987. Bisikalo D.V., V.I. Shematovich, J.-C. Gerard, M. Meurant, S.B. Mende, and H.U. Frey, Remote sensing of the proton aurora characteristics from IMAGE-FUV, Annales Geophysicae, 21, 2165-2173, 2003. Burch, J.L., Lewis, W.S., Immel, T.J., Anderson, P.C., Frey, H., Fuselier, S.A., Gerard, J.C., Mende, S.B., Mitchell, D.G., and Thomsen, M.F.: Interplanetary Magnetic flield control of afternoon sector detached auroral arcs, J. Geophys. Res., 107,1251,10.1020/2001JA007554, 2002. Feldstein, Y.I. and Galperin, Y.I.: The auroral luminosity structure in the High-Latitude Upper atmosphere: Its dynamics and relationship to the large-scale structure of the Earth’s magnetosphere, Rev. of Geophys., 23, 217, 1985. Gussenhoven, M.S., Hardy, D.A., and Heinemann, N.: The equatorward boundary of auroral ion precipitation, J. Geophys. Res., 94, 3273, 1987. Hardy D.A., M.S. Gussenhoven, and E. Holeman, A statistical model of auroral electron precipitation, J. Geophys Res., 90, A5, 4229-4248, 1985. Hardy D.A., M.S. Gussenhoven, and D. Brautigan, A statistic model of auroral ion precipitation, J. Geophys Res 94,370-392,1989. Immel, T.J., Mende, S.B., Frey, H.U., Peticolas, L.M., Carlson, C.W., Gerard, J.C., Hubert, B., Fuselier, S., and Burch, J.L.: Precipitation of auroral protons in detached arcs, Geophys. Res. Lett., 29 10 1029/2001GL03847 2002 . Lilensten J. and M. Galand, Proton-electron precipitation effects on the electron production and density above EISCAT (Tromso) and ESR, Ann. Geophysicae 16, 1299-1307, 1998. Senior, C., J.R. Sharber, O. de la Beaujardiere, R.A. Heelis, D.S. Evans, J.D. Winningham, M. Sugiura and W.R. Hoegy, E and F region study of the evening sector auroral oval: a Chatanika/Dynamics Explorer2/NOAA6 comparison, J. Geophys. Res., 92, 2477, 1987. 126