| Project/Area Number |
15340064
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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 |
Astronomy
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| Research Institution | Kyoto Pharmaceutical University |
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Principal Investigator |
KOIKE Chiyoe Kyoto pharmaceutical University, Pharmacy, Professor, 薬学部, 教授 (20097835)
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| Co-Investigator(Kenkyū-buntansha) |
SUTO Hiroshi National Astronomical Observatory of japan, Assistant professor, ハワイ観測所, 主任研究員 (50300710)
TUCHIYAMA Akira Osaka University, Earth and Space Science, Professor, 大学院・理学研究科, 教授 (90180017)
OKUDA Haruyuki Institute of Space and Astronautical Science, Professor, 宇宙科学研究本部, 名誉教授 (50025293)
FUKADA Mamoru Kyoto pharmaceutical University, Pharmacy, Assistant Professor, 薬学部, 助教授 (00097841)
UMEMOTO Kouitiro Kyoto pharmaceutical University, Pharmacy, Lecturer, 薬学部, 講師 (80097831)
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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 |
¥14,300,000 (Direct Cost: ¥14,300,000)
Fiscal Year 2005: ¥1,700,000 (Direct Cost: ¥1,700,000)
Fiscal Year 2004: ¥3,000,000 (Direct Cost: ¥3,000,000)
Fiscal Year 2003: ¥9,600,000 (Direct Cost: ¥9,600,000)
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| Keywords | circumstellar dust / optical constants / low temperature / fine particles / olivine / forsterite / peak position / half width / 遠赤外スペクトル / オリビン / ピーク半値幅 / バルクの反射率 / 炭酸塩鉱物 / 分光形 |
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| Research Abstract |
For various candidates materials for circumstellar dusts, we investigated the temperature effects on infrared spectra of fine particles. Especially, as for temperature effects on spectra of olivine particles cooling down from room temperature to about 10 K, the intensity and half width of each peak became strong and narrow, respectively, and the position of each peak shifted to shorter wavelength. These tendencies were gentle in mid infrared region, but were very distinct in far infrared region. In particularly for the case of forsterite, the position and half width of 49 and 69μm were shown to be become the temperature indicator. That is, any observer can know the dust temperature from the observed position and half width in circumstellar or interstellar region.
We synthesized olivine samples near end member of forsterite and made clear that the 49 and 69μm peak changed drastically according to the Fe content. Further we synthesized silicate crystalline including Ca, Na, Al elements, a
… More
nd the correlation between peak position and composition was made clear. Amorphous silicates with chondritic components were synthesized by Sol-Gel method, and the process to crystallization was made clear studying the change of infrared spectra after annealing.
As for bulk sample of forsterite, we can obtained the satisfactory optical constants for each axis from each measured reflectance in mid and far infrared. Further, cooling the bulk sample of forsterite continuously to about 10 K, the reflectance were measured in mid and far infrared region for 3 axis. Then, we obtained the optical constants for each axis from the reflectance at many low temperature. As for the reflectance of 69μm band, the intensity become 3 times at 10 K compared to at room temperature. Another peaks at far-infrared also showed similar tendencies. We made clear the optical constants for each axis depend on temperature. From the optical constants, anyone can calculate the spectra in various shape such as needle, oblate, prorate and pale. The shape effects were ascertained in laboratory in the case of ellipse and cauli flower of forsterite. Less
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