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.

V.H. Guineva at al. For this purpose the data from simultaneous measurements of the All-Sky Imagers at And 0 ya Rocket Range (ARR) and at the Auroral Observatory, Longyearbyen, have been compared with plasma and solar wind magnetic field data from the WIND satellite and data from the ground-based magnetic stations from the IMAGE network. Data used We used the following criteria for data selection: 1) Presence of 5577 A and 6300 A intensity measurements; 2) Presence of high-speed stream of the solar wind - a recurrent stream (this was controlled by WIND satellite data); 3) Presence of a substorm at the relevant station (controlled by the IMAGE magnetometers stations chain); 4) All-sky camera observations, presence of aurora and development of a substorm in aurora; 5) Clear sky (no clouds). Data during two recurrent streams from the observational season 2005-2006 have been used: the recurrent stream on 2-9 November 2005 and the one on 23-28 January 2006. The measurements during 3 substorms at Andenes on 3 November 2005 and 4 substorms at Andenes and Longyearbyen on 26 January 2006 have been examined. Only 2 substorms at Andenes on 3 November 2005 and 2 substorms at Longyearbyen on 26 January 2006 satisfy our selection criteria. Results In Figures 1 and 2, the dynamics o f the red and green lines and their ratio during the substorms on 3 November 2005 at Andenes is shown. These substorms developed during the recurrent steam on 2-9 November 2005, the solar wind parameters have the following values: Vx ~ -650 km/s, Bz ~ -4 nT. The upper panel shows the substorm development by chosen images of the red (up) and green (down) lines intensity taken from ASI. The edges o f the row images are cut and they are centered towards the station. Data interpolation is performed to obtain the intensities in 467x467 equidistant points. North direction is marked by an arrow. The black point indicates the station zenith. The bottom panels show the course of the 5577 A, 6300 A emissions and their ratio I6 3 ot/l 5577 during the substorm development. For the emissions intensities and the corresponding ratio, data of the 5577 A intensity in the station zenith and the 6300 A intensity on the same geomagnetic line as the 5577 A one are used. Black arrows point in the graphs to the moments presented in the images in the upper panels. The first substorm is observed from Andenes in 18:35:41 UT (Figure 1, upper panel). The auroral bulge reached zenith at 18:37:20 UT and after that went beyond the station, the latter staying inside the auroral bulge. The ratio I 6300 /I 5577 = 0.031 at the polar edge of the auroral bulge and I 6300 /I 5577 = 0.2 inside it. A N D UT: 18:36.0! 18-37:01 18:37:31 18:38:02 6300 A P ' I 5577 A Я i F ig. 1. The first substorm on 3 November 2005 at Andenes. The upper panel shows the substorm development by chosen images of the red (up) and green (down) lines intensity taken from ASI. The arrow on the left image points to the North direction. The bottom panel presents the course of the green and red line intensities and their ratio during the auroral bulge development, observed in the station