Response of ionospheric electric fields to variations in the interplanetary magnetic field
The STARE system (Scandinavian Twin Auroral Radar Experiment) provides estimates of electron drift velocities, and hence also of the electric field in the high-latitude E-region ionosphere between 65 and 70 degrees latitude. The occurrence of drift velocities larger than about 400 m/s (equivalent to...
| Main Authors: | , |
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| Format: | Article |
| Language: | English |
| Published: |
Copernicus Publications
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| Series: | Annales Geophysicae |
| Online Access: | http://www.ann-geophys.net/14/794/1996/angeo-14-794-1996.html |
| Summary: | The STARE system (Scandinavian Twin Auroral Radar Experiment) provides estimates of electron drift velocities, and hence also of the electric field in the high-latitude E-region ionosphere between 65 and 70 degrees latitude. The occurrence of drift velocities larger than about 400 m/s (equivalent to an electric field of 20 mV/m) have been correlated with the magnitude of the Interplanetary Magnetic Field (IMF) components <i>B<sub>z</sub></i> and <i>B<sub>y</sub></i> at all local times. Observation days have been considered during which both southward (<i>B<sub>z</sub></i>&lt;0) and northward (<i>B<sub>z</sub></i>&gt;0) IMF occurred. The occurrence of electric fields larger than 20 mV/m increases with increases in <i>B<sub>z</sub></i> magnitudes when <i>B<sub>z</sub></i>&lt;0. It is found that the effects of southward IMF continue for some time following the northward turnings of the IMF. In order to eliminate such residual effects for <i>B<sub>z</sub></i>&lt;0, we have, in the second part of the study, considered those days which were characterized by a pure northward IMF. The occurrence is considerably lower during times when <i>B<sub>z</sub></i>&gt;0, than during those when <i>B<sub>z</sub></i> is negative. These results are related to the expansion and contraction of the auroral oval. The different percentage occurrences of large electric field for <i>B<sub>y</sub></i>&gt;0 and <i>B<sub>y</sub></i>&lt;0 components of the IMF during times when <i>B<sub>z</sub></i>&gt;0, clearly display a dawn-dusk asymmetry of plasma flow in the ionosphere. The effects of the time-varying solar-wind speed, density, IMF fluctuations, and magnetospheric substorms on the occurrence of auroral-backscatter observations are also discussed. |
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| ISSN: | 0992-7689 1432-0576 |