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.

following these lines to the tail region and actually it is not clear whether they are going to the polar oval or they are returning back to the solar wind. RESULTS. The pattern of open magnetic field lines sites on the dayside magnetopause for selected values of an interplanetary magnetic field are presented as a- first result of this study (Pig. 3,4). Pictures corresponding to north and south IMF directions are demonstrated. It is worth noting that untiparallel direction of the inner and outer fields is not a sufficient con dition for field lines merging. The comparison with the Luhmann et al. work shows that the sites of the untiparallel lines roughly contain the region of open lines but they are not identical. We have to note that the region about the cusps is deliberately not detailed in these preliminary results because it is not precisly enough computed. Fig. 3. A view on the day side magnetopause from the sun. The shaded region corresponds to open field lines, going to the polar cap. Interplanetary magne tic field, has components В =0, В =0, В =-1.0x ia towards the Sun, Oz is to North and Oy is to dawn. VW ”A ~ °Pen field lines II I ‘I - field lines unlinked to the Earth - lines, crossing the dawn-dusk plane Fig. 4. The same as in the previous figure. The IMF vector here is (0, 0, 1).