Physics of auroral phenomena : proceedings of the 33rd Annual seminar, Apatity, 02 - 05 March, 2010 / [ed.: A.G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2011. - 206 с. : ил.

I. Shagimuratov at al. In the figure it is clearly seen that during the quiet day intensity and number o f irregularities are low against to the disturbed day. The picture demonstrate that similar to auroral oval we can speak about irregularity oval (Aarons, 1997) MCM4 (-79.99; 322.95), July 21-2,7, 2004 ij30 §25 ?20 115 §10 £ 5 a 0 1 30 |25 - ?20 115 §10 £ 5 u 0 rfull. - 4 > - I - I - , . I*- |^f* |**ТЦ 'iS; ~ ■-! - T t # I _Tt-—I__ I— I_rf- RESO (83.10; 320.28), July 21-27, “=*^1- - ■ь- i - 2004 I* l^r— l»rr-»U I— r ^ ~ - r ^ --J = ~ :v ~ ~~S’ -"Z. ~ Л - *r * •" — “* - " ^ r * ~J ~ h r r - i --i .*—:--1—I--1—I__ L i.1__Lt-Г 1—1 1—■Tr ,=Г- • 30 g ;—_ 251- 201 15i 1 0 :- 5I=o- r r— _ 3v+ST _ ^гг __ -5Г j i -=3 ^ - Р ё - f e MAC1 (-64.18; 247.49) Relation between irregularities oval and auroral ovals As we know that auroral ovals are conjugated (Feldstein et al, 1973) we can suppose conjugancy o f irregularities oval too. We should just to know relationship between different ovals. Distribution o f numbers of TEG fluctuations have oval symmetry too (fig. 2). Lets see as a sample the measurements o f TEC fluctuaton at Antarctic stations and compare that with the auroral oval from (Zverev V.L, Starkov G.V. 1975) for events 6-10.10.2004. The Antarctic GPS-data shows strong TEC fluctuations observed at the Antarctic stations CASI, DAVI and MCM4 of 6-10 November, 2004 (Fig. 3). These fluctuations have been associated in (Shagimuratov et al, 2006) with large-scale ionosphere irregularities and polar patches in TEC. We consider that these phase fluctuations could relate directly to electron density irregularities inside the auroral oval. It is perfectly shown in (Aarons et al, 2000) through a similar dependence of the auroral activity and TEC on the magnetic storms development. It is also confirmed by the comparison of the aurora distribution in the oval (Feldstein et al, 1974, Zverev and Starkov 1975) and the TEC measurements by GPS-receivers (Shagimuratov et al, 2006). To understand the dependence in the case considered, we show the oval features by the azimuth diagrams presented in Fig. 5a,b. The diagrams are obviously similar because there are the day-night asymmetry in spatial distribution of the number of phase fluctuations (Fig. 4) and the similar asymmetry in the distribution o f the areas covered by the auroral oval in a case study. The maximum number o f fluctuations is concentrated near the midnight sector of the oval, where it has maximum thickness. The circular azimuth diagrams show a normalized distribution of the fluctuation number in 30' sectors (Fig. 5a) and the normalized areas occupied by the auroral oval in the same sectors (Fig. 5b). This picture is much better for comparison o f auroral and TEC ovals because a different position of both ovals in latitude does not count. _ ЯП- -4— i ■ _ - k C - - * C - - I* ■ I I __“ изо 125 ?20 115 §10 £ 5 u 0 530 |25 щ20 115 §10 £ 5 u 0 230 §25 S20 ^15 $10 £ 5 ® 0 FAIR (64.95; 264.67), July 21-27, 2004 v T - —i - -Д - F I' j) н rJ& # - l - ‘t - l - _L____r I—I I I I-1 * % • - - i b s * * ~ i n~* -IH r r i JOEN (58 36; 108.44), July 21-27, 2004 J — I r i_ rt— I r IJ - — I r l_ rf— l Г l iH - j —-=*_^ -=<!_-i= r~ ^ J ^ J r . I f - * ^ - L - J f - * - \- = J “ ~ y = j . “ ~ _1_-И l . . . l~ l^ 4 Г п - 1 I I I— I i” [— I— I ■ — +- I_I—I _11 ’ I— ' KERG (-58.29; 123.33), July 21-27, 2004 1 - L J M t " I__I— I t - ' U P I 4 - L W ' ■ T:' w-i t o - + c_ I **- — t~ ~~ — ■ - r l -|-i i 1 >— i J __L 12 12 12 0 12 Uni versal 0 12 Time 12 12 2 * Fig 1. a) Variations of Bz and TEC fluctuations occurrence over geomagnetic conjugated polar cap stations MCM4 (south) - RESO (north), b) TEC fluctuations occurrence for auroral MAC1 (south) - FAIR (north) stations, c) Subauroral JOEN (south) - KERG (north) stations. 152