| Project/Area Number |
09440172
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| Research Category |
Grant-in-Aid for Scientific Research (B).
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Space and upper atmospheric physics
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| Research Institution | Nagoya University |
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Principal Investigator |
OGINO Tatsuki Nagoya University, Solar-Terrestrial Environment laboratory, Professor, 太陽地球環境研究所, 教授 (00109274)
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| Co-Investigator(Kenkyū-buntansha) |
NISHITANI Nozomu Solar-Terrestrial Environment Laboratory, Nagoya University, Research Associate, 太陽地球環境研究所, 助手 (10218159)
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| Project Period (FY) |
1997 – 2000
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| Project Status |
Completed (Fiscal Year 2000)
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| Budget Amount *help |
¥11,200,000 (Direct Cost: ¥11,200,000)
Fiscal Year 2000: ¥1,900,000 (Direct Cost: ¥1,900,000)
Fiscal Year 1999: ¥1,800,000 (Direct Cost: ¥1,800,000)
Fiscal Year 1998: ¥2,400,000 (Direct Cost: ¥2,400,000)
Fiscal Year 1997: ¥5,100,000 (Direct Cost: ¥5,100,000)
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| Keywords | solar wind-magnetosphere interaction / magnetohydrodynamics / MHD simulation / magnetosphere ionosphere coupling / interplanetary magnetic field / Jovian magnetosphere / magnetic reconnection / parallel computation |
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| Research Abstract |
We have constructed a 3-dimensional global magnetohydrodynamic (MHD) model to self-consistently treat the solar wind-magnetosphere-ionosphere interaction, and have studied the transfer processes. Configuration and dynamics of the earth's magnetosphere are strongly affected by variations of the solar wind and interplanetary magnetic field (IMF) for recent several hours. Directly driven process on the magnetosphere like a polar electric potential responds in about 10 minutes to their variations, on the other hand loading-unloading precess like onset of tail reconnection in the plasma sheet usually needs about 1 hour time delay from sudden southward turn of IMF.Therefore, it is necessary to know the present magnetospheric configuration as well as the present parameters of the solar wind and IMF in order to obtain future magnetospheric configuration.
Magnetosphere and ionosphere coupling is one of important processes. In order to include the ionospheric feedback process to the global MHD si
… More
mulation of the solar wind-magnetosphere interaction, field aligned currents are traditionally mapped from the inner boundary of magnetosphere onto the ionosphere, electric potential is calculated in the polar ionosphere by including ionospheric conductivity, and then convective electric fields are reversely mapped to the inner magnetosphere. We have tried the opposite procedure in our global MHD simulation.
A 3-dimensional global MHD simulation of the interaction between the solar wind and the earth's magnetosphere has been executed to study the event of November 17, 1996 and the space weather "electrojet challenge" event of March 19-20, 1999. As input for the simulation, one minute values of solar wind parameters from the WIND and ACE satellites were utilized, namely the x-component of the solar wind velocity, the solar wind density, the plasma pressure and the y-and z-components of the IMF in solar-magnetospheric coordinates. We presented cross sectional profiles of energy in the noon-midnight and equatorial planes, polar plots of ionospheric potential and configuration of magnetic field lines every 10 minutes to compare with the satellite and SuperDARN observations. Less
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