1986 Fiscal Year Final Research Report Summary
Studies on Activities of the Jovian decametric Radiations Using the 50 km Mesh Baselind Interferometer
| Project/Area Number |
59420014
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| Research Category |
Grant-in-Aid for General Scientific Research (A)
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| Allocation Type | Single-year Grants |
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| Research Field |
Space and upper atmospheric physics
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| Research Institution | TOHOKU UNIVERSITY |
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Principal Investigator |
OYA Hiroshi Tohoku University, Department of Geophysics, 理学部, 教授 (80025931)
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| Co-Investigator(Kenkyū-buntansha) |
TAKAHASHI Tadatoshi Tohoku University, Department of Geophysics, 理学部, 助手 (80004406)
MORIOKA Akira Tohoku University, Department of Geophysics, 理学部, 助教授 (50004479)
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| Project Period (FY) |
1984 – 1986
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| Keywords | Jovian Decametric Radio Waves / Jovian Magnetosphere / Plasmasphere of Jupiter / Very Long Baseline Interfenometer / Planetary Magnetosphere / 惑星プラズマ |
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| Research Abstract |
Long baseline interferometer with spacing of 50 km range have been developed for the measurements of source positions of the decametric wave radiation from Jupiter. The long base line interferometer system which consists of three observation stations with distances 75 km between Kawatabi and Zao, 45 km between Kawatabi and Yoneyama, and 83 km between Yoneyama and Zao, have been established by producing the Yoneyama stations.
The interferometer system has been designed so as to have the accuracy of 0.5 arc sec, corresponding to 1500 km resolution at Jupiter. Observations using this 50 km base line interferometer system provided data which show the characteristics of sources at Jupiter as
<i> ) The sources related to Io-A is located steadily at south magnetic pole region.
<ii> ) The sources related to Io-B and Io-C indicate apparent switching of the source positions between the north and south poles with period of a few minutes.
The results of the polarization measurement which has been carried out simultaneously with identification of the source position indicate that the Jovian decametric radiations take place in the form of the L-O mode which is expected from the standpoint of the conversion theory for the generation of the planetary radiation.
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