| Project/Area Number |
09640321
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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 |
Astronomy
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| Research Institution | KOBE UNIVERSITY |
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Principal Investigator |
NAKAGAWA Yoshitsugu Kobe University, Faculty of Science, Professor, 理学部, 教授 (30172282)
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| Co-Investigator(Kenkyū-buntansha) |
MATSUDA Takuya Kobe University, Faculty of Science, Professor, 理学部, 教授 (20026206)
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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 |
¥2,900,000 (Direct Cost: ¥2,900,000)
Fiscal Year 1998: ¥1,100,000 (Direct Cost: ¥1,100,000)
Fiscal Year 1997: ¥1,800,000 (Direct Cost: ¥1,800,000)
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| Keywords | Origin of Solar System / Solar Nebula / Protoplanetary Disk / Dust Settling / Planetesimal / Planetary Formation / Planetary Accumulation / Thermal radiation / ダスト沈澱 / 原始惑星系円盤 / ダスト / フラクタル / フラクタル形状 |
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| Research Abstract |
Settling of dust particles caused by vertical component of the solar gravity is an important process in a solar nebula in advance of planetary accretion. We examined the settling and coagulation of dust particles in the solar nebula, taking into account fractal-like morphology of dust aggregates. We found that dust aggregates can keep fractal morphology just for early stages and soon recover the fractal dimension D of three and, hence, the settling time and the final sizes of dust aggregates are quite similar to those obtained by Nakagawa et al. (1986) who did not consider the fractal-like morphology of dust aggregates and always assumed spherical particles. However, the feature of settling is different from the case of D "*" 3 ; in early stages dust aggregates grow up to larger size without appreciable settling, while in the recovery phase toward D = 3 settling accelerates and dust growth decelerates because of rapid increase of the internal density of dust aggregates. This is the reason why there is no appreciable difference in settling time and the final radii between the cases of D <less than or equal> 3 and D "*" 3. As for the question whether the gravitational instability really occurs in the dust layer or not, we have not got the final conclusion yet. So we will continue our
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