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.

I. M. Podgomy and A. I. Podgomy 1 10'' '</) 10'J £о 10‘: o> <D 10“ 10'1 — NOAA 11158 X2.2 S 20W 10 h . O.S-4-OAGOES12 February 15, 2011. 00:00 03:00 06:00 В LINE-OF-SIGNT LB=1.25kG 01:45:45 .^,-12230 B ,m„= 1511G <1>N= 1.318«1022G cm2 <t>s= 1.335«1022G cm2 =1256 G ...им B i* ,,B1500G Фм= 1.329 x 1022G cm2 <t>s= 1.330*1022G cm2 Fig. 3 Above - X-rays of the X2.2 flare according to SDO. Below - the distributions o f the measured (sight- of-line) component o f the magnetic field at the flare maximum obtained with 90 с interval and the difference between them. Magnetic field distribution remains constant during the flare. 07-03-2012 00:02:15 LB=1250 G NO FLARE 08-03-2012 12:02:15 LB=1250 G 07-03-2012 00:24:00 LB=1250G t-B=1250 G 08-03-2012 12:24:00 LB=1250 G LB=1250 G Fig. 4 The distributions of the measured line-of-sight component o f the magnetic field obtained during the X5.4 flare and during quiet time 36 h after this flare. The distributions are obtained with 22 min interval, and the differences between them are shown. Another example o f conservation of magnetic field distribution and the magnetic flux of the active region is shown in Fig. 4. The X5.4 flare is occurred in AR NOAA 11429. This flare duration exceeds 30 min. The distributions of the magnetic field taken at intervals of 22 minutes during the flare and during the quiet state of the Sun 36 hours after the flare is appeared. No characteristic features are seen in the dynamics o f the magnetic field distribution in AR and the magnetic flux during the flare. In both cases, the distribution of the field and the magnetic flux on the solar surface are conserved up to three decimal places. Fig. 5 a). Magnetic field lines of two fluxes in vacuum, b). Flowing-up magnetic fluxes in high conductive plasma, c). The magnetic fluxes interaction creates a current sheet in the corona. Current directions are shown by circles.