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.

Reflection o f the dynamics o fSolar plasma flows in the wavelet skeleton patterns fo r near space parameters In the future work of the classification algorithm for each flow value of E for the two scale fluctuations (up to 300 s and 1500 s) is calculated and for each pair of parameters: B-Bx; B-By; B-Bz; BN; BV; ВТ; Bx-By; Bx-Bz; Bx-N; Bx-V; Bx-T; By-Bz; By-N; By-V; By-T; Bz-N; Bz-V; Bz-T; N-V; N-T; V-T. Thus, each event next parametric row containing 21 (the number of combinations of pairs of parameters) x 2 (number o f investigated scales) = 42 values is described. 4. Classification algorithm and the results of its application The first stage of the classification algorithm identified all possible combinations o f pairs of parameters (B, Bx, By, Bz, N, V, T - 21 combination) in each type o f flow (CIR, Shock, MC, HSS). Next, we calculated the total standard deviation of E over all the experiments separately for the high-frequency (with periods up to 300 sec) and low frequencies (with periods up to 1500 sec). As a result, for each type o f flow two different parametric vector for analyzed scale fluctuations E 300 and E 1500 were obtained. Each vector contains 21 values. At the second stage of the classification algorithm all the possible combinations o f pairs o f flows types (Shock- CIR; Shock-HSS; Shock-MC; CIR-HSS; CIR-MC; HSS-MC - 6 combinations) was identified. Next, we calculated the difference between the modules of the corresponding vectors E 300 and E | 500 and performed normalization of the resulting series of data. Visualization of the normalized difference vectors modules E 300 and E15oo in Figure 3a and 3b is shown, respectively. In other words, there are sets of pairs of spectral images o f PSW and the IMF, which are different (closer to 100%) or similar (closer to 0%) flow types. We have proposed a statistically significant 75% threshold above which ensures appropriate differentiation of plasma formations within certain parameters. 100 90 80 70 60 50 40 30 20 10 0 A) ■ s-dr os-hss ss-m c ocir-hss acir-mc ahss-mc z > К oq m со cT i x x x lr > . > > ^ N N X X rn fl] CD > ro 03 Ш ш CD CD £0 CD > br Z Z > 100 90 80 70 60 50 40 30 20 10 0 B) is-cir Ds-hss gs-m c ocir-hss Bcir-mc Ehss-mc !, x > 2* Z > H- > N Z > H CD CD CD .i ' CD CD i i • * ■ 1 cQ CD CD i i x X X cd cn cd ш ш x X j Q t a m Z > ь > > > N N N CD CD CD CD CD CD Fig. 3 75% C o m b in atio n s o f p a ra m e te rs C o m b in a tio n s o f p a ra m e te rs The normalized difference between the modulus of E300 (a) and E1500 (b). The horizontal line corresponds to The results in Table 1 as combined are shown. S hock C IR H S S M C S h o ck N -V ; B -B x; B x-V ; N -V ; N -V ; C IR B-By; Bz-N ; N -V ; V -T; B x-V ; B x-B y; HSS B-By; Bx-V ; N -V ; Bx-V; B x-B y; B x-V ; B y-B z; M C N -V ; Bx-By; B x-N ; N -V ; B x-V ; B y-Bz; Table 1. The intersections of rows and columns show the sets of pairs of spectral images o f PSW and IMF, which are different types of flows (by 75% or more) - on a white background for high-frequency part with periods up to 300 seconds, on a gray background - for the low periods up to 1500 seconds. 128