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.

“Physics o fAuroral Phenomena", Proc. XXXV Annual Seminar, Apatity, pp. 37 - 40, 2012 © Kola Science Centre, Russian Academy of Science, 2012 Polar Geophysical Institute WAVELET COMPONENT MANIFESTATION OF SOLAR WIND PARAMETER DISTURBANCES WHICH CORRESPONDING TO THE PLASMA FLOWS AT THE DYNAMICS OF MAGNETIC DISTURBANCE SPECTRUMS ALONG THE GEOMAGNETIC MERIDIAN N.A. Barkhatov1’2, S.E. Revunov1, D.V. Shadrukov1 'Nizhniy Novgorod State Pedagogical University, Nizhniy Novgorod, Russia 2Nizhniy Novgorod State Universityfo r Civil Building, Nizhniy Novgorod, Russia Abstract. The study a parallel analysis of the results of the post-processing of the wavelet components for low frequency (LF) disturbed parameters of the Solar Wind plasma flows and disturbances of the horizontal component of the geomagnetic field (range of hydromagnetic waves) recorded along the meridional chain of stations in different strength of geomagnetic storms is devoted. The dynamics of the components of the spectrum of perturbations of the Solar wind meeting the Solar flux in the low-frequency (2-8 MHz) spectrum of magnetic disturbances at high- latitude stations is shown and as a diagnostic tool of the plasma flow can be used. 1. Introduction Previously, that the LF oscillations of Solar Wind parameters are shown in the records of magnetograms on ground- based observatories was observed [Gul'el'mi and Troickaja, 1973]. The main objective of the study is to test the possibility of establishing type approached to the magnetosphere disturbed flows Solar Wind on basis of analysis of the components of the wavelet spectra of the near-Earth space environment parameters and components of geomagnetic field along the high-latitude part of the meridional chain of stations is consist [Barkhatov et al., 2011]. This approach to test the hypothesis, that in period geomagnetic storms, created Solar plasma flows, some of the magnetic LF disturbance on the Earth surface associated with MHD disturbances in these flows and penetrates into the magnetosphere from the Solar Wind is used. In this special attention spares to high-latitude regions, where the configuration of the geomagnetic field of LF oscillations of the Solar Wind into the Earth's magnetosphere may allow direct penetration. 2. The data used and processing techniques In study minutes data for geomagnetic field components from a grid of stations IMAGE (http://www.geo.fmi.fi/image) and the data for parameters of Solar Wind (PSW) and the interplanetary magnetic field (IMF): Bz, N, P и VBz (http://cdaweb.gsfc.nasa.gov) was used. Data intervals to 12 daytime intervals magnetospheric storms of varying intensity on the index Dst indication (http://spidr.ngdc.noaa.gov/spidr/) are correspond and between 2000 and 2003 are recorded [. Barkhatov et al, 2011]. Solution to the problem of identifying the type who approached magnetosphere disturbed Solar Wind on its expression in the records of magnetograms on ground-based observatories difficult in obtaining quantitative estimates of consistency studied spectrums. To successfully assess the consistency spectral pattern only the key features should contain [Astafieva, 1996]. This aim by calculating the corresponding wavelet skeletons and further matching can be achieved. In this study the algorithm for this approach was suggested. The conclusion for the consistency of any pair of skeletons on minimizing the mean square deviation on the registration of the local maxima of the spectrum (representing skeletons) is based. To do this, the coordinates of points on the x-axis (time) determine X - [x, x2 ... ] and у-axis (frequency) Y = [>’1 y 2 f°r skeleton in his frame is forming. For each pair of skeletons the standard deviation is calculates like this f l ~ ZK -* ?2) , n M where n - the number of points that form the skeleton (in our experiments n = 23), si, s2 - indexes of belonging to the skeleton of the selected pair. Then the deviation of convenience by the total maximum value of the sample is normalized. Dxn = max (Dx) • 100 % 37