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Response of the reconnection electric field and polar cap potential to the IMF and velocity of solar wind
Authors:Keiichiro Fukazawa  Tomoharu Aoyama  Tatsuki Ogino  Kiyohumi Yumoto
Institution:1. Department of Earth and Planetary Sciences, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan;2. Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan;3. Space Environment Research Center, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan;1. State Transport University, 9 Moskovsky Av, Saint Petersburg 190031, Russia;2. Geophysical Center of the Russian Academy of Science, 3 Molodezhnaya Str, Moscow 119296, Russia;3. Space Research Institute of the Russian Academy of Science, 84/32 Profsoyuznaya Str, Moscow 117997, Russia;1. Department of Petroleum Engineering, Amirkabir University of Technology, Tehran, Islamic Republic of Iran;2. Institute of Geophysics, University of Tehran, Tehran, Islamic Republic of Iran;3. Department of Mining and Metallurgical Engineering, Amirkabir University of Technology, Tehran, Islamic Republic of Iran;4. Exploration and Production Research Center, Research Institute of Petroleum Industry, Tehran, Islamic Republic of Iran;5. Department of Geophysics, Exploration Directorate, National Iranian Oil Company, Tehran, Islamic Republic of Iran
Abstract:It is well known that the cross polar cap potential is saturated under a strong interplanetary electric field and is often said to be related to the ionospheric currents. To investigate the other factors influencing this phenomenon, a global magnetohydrodynamics simulation not including the feedback from the ionosphere to the magnetosphere was conducted. The simulation results showed that an increase in the southward IMF causes a smaller increase in the cross polar cap potential than that caused by an increase in the solar wind velocity. This difference was caused by the transportation of reconnected magnetic field lines towards the tail.
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