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.

requirement for associated D-component of magnetic field variations (at the ground) to have an amplitude >. 100 nT and duration of 10-15 min. EXPERIMENTAL DATA. First of all let us recollect v/hat kind of a structure of fields and particle precipitation in the ionosphere is connected with the region of the localized Upward FAO j* of the substorm current wedge. Westward of current a great positive deviation of the magnetic field D-component is observed on the ground. Just behind a bright WTS in the region of intense energetic particle precipitation, i.e. in the active region drastically differ ent from the former one, the D-component changes its sign /5/. Taking this into account we determine, as in paper /6/, the moment tQ for the considered substorms when the large variations of the D-component in the auroral zone began and the moment t^ when the active region passed the satellite's meridian. Thus during the interval from t to t1 the satellite was located westward of. the current j* region and after t^ it moved more and more to the east. Behaviour of the E-field and energetic proton fluxes in the active region. Figure 1a shows a typical D-component variation on the Earth. The darkened areas denote the regi£>n of active auroras and enhanced fluxes of energetic electron precipitations into the ionosphere. The scheme below demonstrates the behaviour of energetic electron and proton fluxes in the magnetosphere at 6.6 Rg. The azimuthal component of the E^ electric field for five substorms is presented at the bottom of the figure. The Ep record ia broken so as the E-behaviour near distinctive moments tQ , t ^ , tg can be compared for different substorms. The arrows denote the observed Eg meridional component; in the figure the equator- ward direction (as projected on the ionosphere) corresponds to the upward arrow. It has been found /6/ that energetic electron and proton anti correlation near the western edge of WTS is registered both in the vicinity and well inside the trap ping region (Ja = J„ and > J„ respectively). In Fig.1a to J„ relation for energetic elect rons is given for t=tQ . Fig.1a reflects the main feat ure in E-field distribution in the magnetospheric active region, i.e. the change of the direction of the E q azimuthal component is colloca ted with the fronts of energetic proton fluxes. When proton fluxes grow the ED direction changes from westward to eastward, whereas the opposite change of the E D directi on occurs when the proton flux decreases. Fig.1. a - Behaviour of the electric field in the magnetosphere in the vicinity of WTS; b - the signs of charges at the pressure boundary. tp (ti_____ ti ----------- T - y D ontheEarth \ -e dipo illation m m /7 w themagneto sphere : 'V + P + 4 - 4 L § 4 r 5 0 1 — Щ t i Ж - v*rw I * A h March ♦ J r J „ March5 J / > J « J a n u a r y 3 0 J i^ J h < ♦ i r t ■**’ 0 I „ IT [. < 2 . 4 и V ♦ , u - k L 1 ч V J a n u a r y 2 5 J i '- J h west ) ( > с ) F A C b . I i r m t . / , V п л . - y * deficit excett 36