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.

The active region magneticflux correlation withflares appearance boundary conditions. The PERESVET code is used in which the procedure of Laplace equation solving with the oblique derivative is inserted. This method is developed in [10]. The potential field is calculated in big dolmen for to minimize the errors connected with uncertainty of boundary condition in the corona. Such method is available, because the magnetic field distribution on the photosphere is not distorted by a current sheet situated high in the corona. The fig. 2 shows line of sight SOHO MDI distribution and distribution of calculated normal magnetic field, when the active region AR10486 has been located about 30° from the East solar limb. The northern Фм and southern Os magnetic fluxes are shown below. The calculations have been carried out in the domain 4Ю 10 см x 4Ю 10 cm , when the active region is displaced from the East limb in ~30°. The figure shows that the line-of sight magnetic field distribution is rather different from distribution of the normal magnetic component. Ф м =4.2-1022М х Ф5=2.7-1022М х фК|=6.4-1022Мх Ф5=4.1 -1022Мх Fig. 2. a) Line of sight SOHO MDI (http://soi.stanford.edu/magnetic/index5.html, in the active region AR10486 (24.10.2003 19:15). 6 ) Calculated magnetic field distribution o f the normal magnetic field component. For calculation of the normal magnetic field the method o f Laplace equation with inclining derivative solving are used [10]. The area domain 4 xlOlocmx 4 xlOtocm is bigger than the active region, and errors in setting nonphotospheric boundary condition does not influence strongly on results. Such method permits to obtain the normal magnetic component during all time of active region traveling across the solar disk. The active region AR10486 appears on the solar back side. It travels from 26.10.2003 to 3.11.2003 on the visible disk. Evolution o f the normal North and South magnetic flux components are shown in fig. 3. х Ю ^ М х • Ф м о ф 8 AR 1 0 4 8 6 89