Physics of auroral phenomena : proceedings of the 37th Annual seminar, Apatity, 25 - 28 February, 2014 / [ed. board: A. G. Yahnin, N. V. Semenova]. - Апатиты : Изд-во Кольского научного центра РАН, 2014. - 125 с. : ил., табл.

Northern auroral structures before breakup and solar wind 31.12.2007 Lovozero Intens. arb.units WIND Bx =50 min 2 3 ACE i c • WIND 150 x Re (> Figure 3. Auroral TV and solar wind magnetic data for 31.12.2007. Arc luminosity variations (1, 2) By - components of solar wind magnetic field registered by ACE(3), WIND Bx and By components (4 ),'TV frame example for this date (5) and satellites position (6). The same data for 31.12.2007 are shown on Fig. 3. Good correlation o f arc luminosity variations with solar wind magnetic field is quite visible as well, especially for the time interval of aurora activation about 17 15-17 40 UT. Correlation for 18.35-19.05 UT is rather good for satellite ACE, but not so good for WIND. Besides aurora intensification at 18.05 UT (this moment marked by vertical line about 17.00 UT) is almost invisible in satellite data, though coincide with WIND By magnetic field component increasing. Obviously, all those details of correlation are because of the fact that magnetic field is measured locally, at the point of satellite position but solar wind interaction with magnetosphere definitely has global integral character. 20