Geomagnetic Control on the Equatorial Plasma Bubble Formation

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Attempts have been made repeatedly to investigate the effect of magnetic activity on the equatorial plasma bubble (EPB) generation. At the moment, it is generally accepted that magnetic activity tends to suppress the EPB generation and evolution in the pre-midnight sector. As for the post-midnight sector, it is believed that the EPB occurrence probability will increase after midnight as magnetic activity increases. Moreover, the growth rates of the EPB occurrence probability will strongly depend on solar activity: at the solar activity minimum, they will be the most significant. A sufficient amount of the observations is required to confirm these ideas. For this purpose, the EPB observations obtained on board the ISS-b satellite (~972−1220 km, 1978−1979) in the pre- and post-midnight sectors are best suited. The data were considered in two latitudinal regions: equatorial/low-latitudinal (± 20°) and mid-latitudinal ± (20°−52°) regions. LT- and Kp-variations of the EPB occurrence probability were calculated for both groups. (1) It was revealed that the occurrence probability maximum of the EPBs recorded at the equator and in low latitudes is in the pre-midnight sector. The EPB occurrence probability decreases with increasing Kp index with a delay of 3 and 9 hours before the EPB detection. (2) However, the occurrence probability maximum of the EPBs recorded at the mid-latitudes is in the post-midnight sector. Their occurrence probability increases slightly as Kp index increases, when Kp is a 9-hours delayed one. Thus, the idea of the ionospheric disturbance dynamo (IDD) influence on the post-midnight EPB generation has been confirmed. IDD mechanism sets in after some hours of enhanced geomagnetic activity and favors the generation. However, its influence is weakened during the years of increased solar activity.

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Sobre autores

L. Sidorova

Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of the Russian Academy of Sciences

Autor responsável pela correspondência
Email: lsid@izmiran.ru
Rússia, Troitsk

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2. Fig. 1. LT-variations of the EPB observation probability (RERV). (a) - Equatorial and low latitude region: ± 20°. (b) - Mid-latitude region: ± (20°-52°).

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3. Fig. 2. RERV variations as a function of the interval value of the Kr-index. Equator and low latitude region: ± 20°. (a) - Delay of the Kr-index for 3 hours. (b) - Delay of the Kr-index of 6 hours. (c) - Delay of the Kr-index for 9 hours.

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4. Fig. 3. Variations of RERV as a function of the interval value of the Kr-index. Mid-latitude region: ± (20°-52°). (a) - Delay of the Kr-index for 3 hours. (b) - Delay of the Kr-index for 6 hours. (c) - Kr-index delay for 9 hours.

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5. Fig. 4. Schematic representation of the evolution of equatorial plasma bubbles with respect to magnetic force tubes, dipole latitude, and altitude. Horizontal lines show the approximate flyby altitudes of the ISS-b (~ 972-1220 km), ROCSAT-1 (~ 600 km), and AE-E (~ 350-475 km) satellites.

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