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.

28.9.77 [$0Л«ПкуШ н J r . Sactankyloi 27.6MHz CNA 400 200 Rovanicmi27.6MHz Oulu 27.6 MHz CHA -„E l A L Jyvizsky[a 27.6 MHz i i 12. ? f soatotHkyfa н 27-iMH L 200 3 1 0 600 ; 212.73 SodankylaH Kevo 11 z ш i n 'rд1— Ivato 27.6MHz Ъ CNA Oulu гит см -13 «fT-rfKV'>r-Tnl 1M 15UT Kevo Z H mh z CNA J VlvaCo 27.6MHz CM 3 [ „ Soiankyli 276 MHz L™ CNA Sootankjl.it 27. 6 MHz CNA -« Rovaniemi 27.6MHz w CNA Oulu 27.6 MHz Fig. 11. The same as Pig.Ю on 28 September 1977, 11 December 1977 and 27 February 1976. EASTWARD ELECTROJET AND INTERPLANETARY MAGNETIC FIELD. In one paper Clauer et el./1982/ wrote that the intensity of the westward electrojet better correlates with solar wind energy parameters than the eastward electrojet. From this it should be concluded that rather magnetospheric than inteplanetary processes are responsible for the к-componsnt KAU m 250 -2f0 10 -10 10.12.83 ж-component HuO T f 7 T T T vs £ ^ / / / i t v \ \ f ? ? 'M H generation of the eastward electrojet. This is contradictory to the o p inion that convection or the interplanetary electric field are the only reasonj for the eastward electrojet. According to this, a quite close c o r r e lation between this electrojet and inter planetary energy should be observed. In Fig, 12 and 13, for 4 events of Fig.9 the X component of one s t ation of the EISCAT magnetometer cross is represented together wi t h the B z component of the interplanetary m a g n etic field. It becomes apparent that the two events on July 24, 1983 and on December 10, 1983 for w h i c h - according to Pig. 9 - the position of the eastward electrojet scarcely Fig. 12. Comparison between magnetic X-component and southward component of the interplanetary magnetic field on 24 July 1983 and 10 December 1983. 66