| Project/Area Number |
09640513
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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 |
固体地球物理学
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| Research Institution | The Institute of Space and Astronatical Science |
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Principal Investigator |
MIZUTANI Hiroshi The Institute of Space and Astronatical Science, Research Division for Planetary Science, Professor, 惑星研究系, 教授 (00011578)
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| Co-Investigator(Kenkyū-buntansha) |
HONDA Rie Kochi University, Research Associate, 理学部, 助手 (80253334)
IIJIMA Yu-ichi Research Division for Planetary Science, Research Associate, 惑星研究系, 助手 (80300698)
TANAKA Satoshi Research Division for Planetary Science, Research Associate, 惑星研究系, 助手 (30249932)
HAYAKAWA Masahiko Research Division for Planetary Science, Research Associate, 惑星研究系, 助手 (40228557)
FUJIMURA Akio Research Division for Planetary Science, Professor, 惑星研究系, 教授 (70173458)
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| Project Period (FY) |
1997 – 1998
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| Project Status |
Completed (Fiscal Year 1998)
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| Budget Amount *help |
¥3,100,000 (Direct Cost: ¥3,100,000)
Fiscal Year 1998: ¥700,000 (Direct Cost: ¥700,000)
Fiscal Year 1997: ¥2,400,000 (Direct Cost: ¥2,400,000)
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| Keywords | moon / ejecta deposits / Clementine spacecraft / multi-band image / lunar suface composition / reflection spectra |
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| Research Abstract |
We established a method of estimating the composition of the lunar deep interior using the UV-VIS data obtained by the Clementine spacecraft. We also made a data base for the UV-VIS images obtained by the Clementine, This system consists of a workstation and a CD-ROM changer which is loaded with about one million Clemetine images. The image data in the data base can be retrieved remotely too through computer network. The data base also allows us to search and inspect the images located in different CD-ROMs. With our data analysis system, we can calculate the latitude and longitude of each pixel in an image using the information listed in the header file which describes the position and attitude of the spacecraft, and then we can automatically assemble many images to make a large mosaic and extract the required information.
In order to extract information of the composition from the visible-infrared data, geometrical corrections such as those of topographic correction and phase angle cor
… More
rection are very important. The study made in the last year showed that we can calibrate the reflection spectra within 3% accuracy if the topographic correction on the reflection spectra is made using the lunar topographic data. We also showed that the effect of the phase angle (i.e. angle between the impinging solar light and reflecting light from the lunar surface) depend on the material and wavelength, In this year's study, we investigated in detail on the phase function using the Clementine data which gives us the multi-spectrum images taken at different phase angles. Through this study, we can demonstrate quantitatively the material and wave-length dependence of the phase angle. The compositional difference between Mare and Highland amounts to the difference of phase function of 17% at a phase angle of 2 deg, and the wavelength difference from 415nm to 7Sonm amounts to 10% at the same condition. From these improvement of analysis method, it has become possible to infer the composition or space erosion effect more reliably than before. Less
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