Physics of auroral phenomena : proceedings of the 36th Annual seminar, Apatity, 26 February – 01 March, 2013 / [ed. board: A. G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2013. - 215 с. : ил., табл.

S.E. Revunov et al. Conclusion According to the modem physical notions about the existence of oscillatory processes in isolated Solar wind structures classification approach to the problem of differentiating types of geoeffective plasma flows was proposed. It is shown that each type of flow is characterized not only a characteristic set of parameters such as velocity, density, pressure, temperature, strength of the magnetic field, as well as the fundamental relationships between these parameters. Such connections in the synchronization parameters associated with the flow of the wave packets are shown. Numerical assessment of the level of pairwise synchronization parameters recorded plasma formation suggests to a particular type it belongs. As a result of the referring of classification algorithm found the following patterns: 1. The identification of flow-type Shock possible to synchronize N-V. 2. The identification of flow-type CIR possible to synchronize oscillations parameter pairs Bx-N, Bz-N. 3. The identification of flow-type HSS possible to synchronize oscillations parameter pair Bx-V. 4. The identification of flow-type MC possible to synchronize oscillations parameter pairs Bx-By, By-Bz. 5. Low-frequency (periods up to 1500 sec) part of spectral disturbances of the PSW and IMF analyzed flows demonstrate their individual character, which actually reflects the duration of the event. High-frequency (periods up to 300 sec) part o f disturbances PSW and IMF analyzed flow separates them only on dynamic characteristics of the Solar wind. 6. In general, the flow type MC characterized by long-term changes. Streams such as CIR can be identified by relatively rapid changes in all parameters in all of the analyzed scale of disturbances. Flows type Shocks cause abmpt changes in all parameters, especially when a low-frequency part of the spectrum analysis. Streams such as HSS can be identified by slow changes in the parameters of velocity, density, temperature, and rapid changes in components of the magnetic field. The results are expected to be tested by events that are not included in this study. A c know ledg em en ts. Thanks to Barkhatov N.A. for the problem and for useful discussions. This work was supported by RFBR grant 12-05-00425 and by the project "Development of modem methods of forecasting the state of the magnetosphere-ionosphere in order to ensure successful communication on the basis of fundamental research of the influence of solar activity" institution o f higher education within the executable tasks of the Ministry of Education and Science. References Steed, K., C.J. Owen, P. Demoulin, and S. Dasso, Investigating the observational sig-natures of magnetic cloud substructure H i. Geophys. Res. -2011. -V .l 16, A01106, doi:10.1029/2010JA015940. Tessein, J.A., C.W. Smith, B.J. Vasquez, and R.M. Skoug, Turbulence associated with corotating interaction regions at 1 AU: Inertial and dissipation range magnetic field spectra // J. Geophys. Res. -2011. —V. 116, A10104. doi:10.1029/2011JA016647 Wawrzaszek, A., and W.M. Macek, Observation of the multifractal spectrum in solar wind turbulence by Ulysses at high latitudes // J. Geophys. R es.-2 0 1 0 .-V .l 15, A07104. doi: 10.1029/2009JАО151 129