Physics of auroral phenomena : proceedings of the 39th annual seminar, Apatity, 29 February-4 March, 2016 / [ed. board: N. V. Semenova, A. G. Yahnin]. - Апатиты : Издательство Кольского научного центра РАН, 2016. - 167 с. : ил., табл.

N. G. Kleimenova et al. After —11.20 UT, the wave polarization suddenly turned to a strong right-hand direction, which can indicate that the ionospheric exit point of wave was nearly overhead or between these stations. We compared the ground-based VLF data with the measurements by THEMIS D (ThD) and THEMIS E (ThE) mission [Angelopoulos, 2008], located in this time in the evening flank of the magnetosphere (Fig. 7). They showed typical behavior of energetic electron and ion fluxes as well as magnetic field variations for SC. The THEMIS В (ThB) satellite (do not shown here) was located in front of the magnetosphere at X=~50 Re and Y=~20 Re. These data demonstrated a sharp particle flux enhancement (typical for SC). LOZ Seuth Tim», mln, from 2014-122911 Л 0 UT Figure 6. The results of the analysis of the LOZ VLF data (interval 11.00-12.00 UT). It is seen (Fig. 7) that the VLF emission onset, associated with SC, coincided with a sharp electron and proton flux increase measured by ThD and ThE spacecraft. Apparent­ ly, that is a result of the electron cyclotron instability [Trakhtengerts and Rycroft, 2008] arising by the compres­ sion-induced changes in the electron phase space density and pitch angle distribution caused by SC [Kennel and Petschek, 1966]. ions Figure 7. The energetic electrons and fluxes, magnetic field and pressure measured by THEMIS D and THEMIS E located in the evening flank of the magnesphere (at X=_7 Re Y=~10 Re) and VLF data at KAN (bottom panels). 38