Solar activity dependence of electron and ion temperatures using SROSS C2 RPA data and comparison with IRI model |
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| Institution: | 1. Space Science and Development Research, Ethiopian Space Science and Technology Institute, Addis Ababa, Ethiopia;2. Washera Geospace and Radar Science Laboratory, Physics Department, Bahir Dar University, Bahir Dar, Ethiopia;3. Climate and Space Sciences and Engineering, University of Michigan, USA;1. West Department of Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS, Kaliningrad 236017, Russia;2. Immanuel Kant Baltic Federal University, Alexandra Nevskogo Str., 14, Kaliningrad 236041, Russia;3. Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS, Troitsk, Moscow Region 142190, Russia;4. Institute of Solar-Terrestrial Physics SB RAS, Irkutsk, Russia;5. Institute for Cosmophysical Research and Aeronomy, Yakutsk, Russia;1. Institute of Ionosphere, National Center for Space Research and Technology, Almaty, Kazakhstan;2. Institute for Physics, Southern Federal University, Rostov-on-Don, Russia;3. Hacettepe University, Dept. of Electrical and Electronics Engineering, Ankara, Turkey |
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| Abstract: | Electron and ion temperature (Te and Ti) data observed using RPA on board SROSS C2 satellite are investigated for the variation with local time, season, latitude (0–30°N geographic) over a half of a solar cycle (1995–2000). The nighttime Te (～1000 K) is independent of the season and the solar flux whereas Ti exhibits positive correlation with the solar activity during all three seasons. In the early morning hours during summer, Te is higher by ～500 K than other seasons in all three levels of solar activity. During winter and equinox in the early morning hours, Te and Ti are higher during low solar activity, showing a negative correlation with solar flux. During daytime, the Ti increases with the solar flux in winter and summer solstice, but is independent in equinox. IRI underestimates Te and Ti during the morning period by 50–75% in the equatorial and near-equatorial stations during all levels of solar activities. |
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