| Project/Area Number |
15540430
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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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 | Kumamoto University |
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Principal Investigator |
SATOH Takehiko Kumamoto University, Faculty of Education, Associate Professor, 教育学部, 助教授 (10297632)
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| Co-Investigator(Kenkyū-buntansha) |
MORIOKA Akira Tohoku University, Faculty of Science, Professor, 大学院・理学研究科, 教授 (50004479)
TOKUMARU Munetoshi Nagoya Univ., Solar Terrestrial Environment Lab., Assoc.Prof., 太陽地球環境研究所, 助教授 (60273207)
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| Project Period (FY) |
2003 – 2005
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| Project Status |
Completed (Fiscal Year 2005)
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| Budget Amount *help |
¥3,600,000 (Direct Cost: ¥3,600,000)
Fiscal Year 2005: ¥1,200,000 (Direct Cost: ¥1,200,000)
Fiscal Year 2004: ¥900,000 (Direct Cost: ¥900,000)
Fiscal Year 2003: ¥1,500,000 (Direct Cost: ¥1,500,000)
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| Keywords | Jupiter / Aurora / Infrared / Solar Wind / Magnetosphere / Ulysses / Interplanetary Magnetic Field / 磁気圏・電離圏 / 超高層大気物理学 / 惑星オーロラ / 光学赤外線天文学 / 宇宙科学 |
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| Research Abstract |
We have investigated the correlation between the solar wind parameters and integrated flux of Jupiter's infrared aurora to find out if they show "positive" or "negative" correlation. In the past, observers suggested "positive" correlations (weak, though), and on the other hand, theoretists proposed models which expect negative correlations between the solar wind and Jupiter's auroral response. This study is to clarify the case using observations and simulations.
The solar wind parameters have been determined based on MHD tomography analysis of interplanetary scintillations which are measured at 4 observing sites in Japan. Parameters on interplanetary magnetic field (IMF) have also been determined. Jupiter data have been selected from our archives and 4 data sets (acquired in 1998-2000) were compared with the solar-wind data.
Our conclusions include :
(1) Two data sets, each of which has many nights of Jupiter observations, indicate a good "positive" correlation with the solar-wind ram pressure.
(2) One data set is indicative of "negative" correlation, however, it includes only 2 nights of Jupiter observations, and lack of IPS measurements just before this period prevents us from solid conclusions. Another set shows nearly constant aurora brightness in spite of a dramatic increase of the solar-wind ram pressure.
(3) Among all of 4 data sets, the aurora brightness can be clearly divided in 2 groups : the first one is "brighter" aurora and is associated to northward IMF, and the second one is "dimmer" aurora associated to southward IMF. Such relationship is consistent with the fact that Jupiter's magnetic field has an opposite polarity compared to the Earth's one.
The last conclusion in the above (correlation with IMF polarity) is the most important and is for the first time indicated based on the observations. With such useful tools, developed through this study, we should be able to continue increasing our knowledge about the solar-wind magnetosphere interactions.
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