Структура и динамика полярных токовых систем : материалы международного симпозиума «Полярные геомагнитные явления», 25-31 мая, Суздаль, СССР / Акад. наук СССР, Кол. фил. им. С. М. Кирова, Поляр. геофиз. ин-т. – Апатиты : [б. и.], 1988.

Pi* 2. Average dependence of AU and Fig.3. Average dependence of AU AL indices on the IMP B a component shown and AL indices on the solar wind separately for different ranges of solar velocity shown separately for wind velocity (Kuznetsov and Sergeev, different ranges of B z (Kuznetsov <nai\ and Sergeev,1981j Murayama et al., 1 9 8 1 b 1980). and AL-indices is leas evident. Investigation of this problem (Kuznetsov and Sergeev,1983; Murayama et al.,1980; Danilov,1981 1 Amezawa and Murayama,1985) has shown that the activity is much higher the larger the velocity of the solar wind, Aocording to Kuznetsov and Sergeev (1981) the level of the magne tic activity under B z > 0 is independent of B z while under B a* 0 the activity is in linear relationship with B z (Pig.2). The threshold value for the change of relation between B_ and activity indices is defined by the solar wind z velocity» В a: 0 under V oul^ 400 km/s, whereas B__ 2 nT under 600 km/s. it U QW « О SW ■Pig.3 represents the relationship between AU, AL indices arid solar wind velooity as a function of B z . This relationship may be considered as a linear one only for sufficiently large values of the IMP southern component B z * -2 nT, while under B z » -2 nT for AL-lndex the dependence is rather quad ratic, AL ~ V 2 (Murayama, 1982). For AU-index Maezawa (1979) finds a linear relationship, AU~-V. According to Maezawa and Murayama (1985) the different dependence of AU and AL indices on the solar wind velooity is representative of different effects of T m in various LT sectors, the strongest effects being in 20.00-24.00 MLT. The dependence of magnetio aotivity on the product of two values, B 0 and V 0W was examined by Murayama (1982), Holzer and Slavin (1982), Meloni et al. II7