The Responses of Ionospheric Conductivities on the Mid-Latitudes to Changes in the B Z Component of Interplanetary Magne
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The Responses of Ionospheric Conductivities on the Mid‑Latitudes to Changes in the BZ Component of Interplanetary Magnetic Field Erdinç Timoçin1 · Ali Yeşil2 · İbrahim Ünal3
© Springer Science+Business Media, LLC, part of Springer Nature 2020
Abstract In this study, we investigate the response of the ionospheric conductivities on the middle latitudes to the southward and northward turnings of the BZ component of the interplanetary magnetic field (IMF). For this purpose, parallel conductivity (σ0), Pedersen conductivity (σ1), Hall conductivity (σ2) data calculated for Rome (41.8° N, 12.5° E); Juliusruh (54.6° N, 13.4° E); Uppsala (59.8° N, 17.6° E); Lycksele (64.7° N, 18.8° E) during the 22nd solar cycle are examined. The superposed epoch analysis method is used to investigate the response of the conductivities to the southward and northward turnings of the BZ component. From the analysis results it is observed that the turnings in the BZ component of the IMF have significant effect on all conductivities. At the event moment (zero time), the southward turnings of the BZ component increases all conductivities while the northward turnings of the BZ component decreases all conductivities. The effect on the conductivities of the changes in the B Z component occurs before about 18 h from the event moment, and this effect disappears after about 24 h from the event moment. Furthermore, all of ionospheric conductivities shows or does less reaction to changes in the B Z component as latitude increase. Keywords Ionosphere · Ionospheric conductivities · Interplanetary magnetic field · Superposed epoch analysis
* Erdinç Timoçin [email protected] Ali Yeşil [email protected] İbrahim Ünal [email protected] 1
Department of Medical Services and Techniques, Mersin University, 33343 Mersin, Turkey
2
Department of Physics, Faculty of Science, Fırat University, 23169 Elazıg, Turkey
3
Department of Science Teaching, Faculty of Education, İnönü University, 44280 Malatya, Turkey
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1 Introduction The interplanetary magnetic field (IMF) is the solar magnetic field carried by the solar wind among the planets of the Solar System. IMF has vector components ( BX, BY, BZ). The BX component is in the ecliptic plane directed along the Sun–Earth line (positive toward the Sun), BY is in the ecliptic plane perpendicular to the Sun–Earth line (positive toward dusk), BZ (the north–south component) is perpendicular to the ecliptic plane and positive to the north [1]. It is well established that the north–south oriented BZ component of the IMF is the most important influence on the magnetosphere and high latitude ionosphere, as it controls the fraction of the energy in the solar wind flow which is extracted by the magneZ tosphere. A negative B Z values increase this energy transfer whereas the positive B component values reduce such an energy input, in particularly at the high latitudes. When BZ is strongly negative, the magnetic reconnection between the IMF a
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