Giant impacts between proto planets and late stage planetary accumulation
| Project/Area Number |
16540382
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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 |
Solid earth and planetary physics
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| Research Institution | Yachiyo International University (2006-2007)
Tokyo Institute of Technology (2004-2005) |
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Principal Investigator |
EMORI Hiroyuki Yachiyo International University, Department of business management, Professor (30262257)
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| Co-Investigator(Kenkyū-buntansha) |
NAKAZAWA Kiyoshi Tokyo Institute of Technology, Graduate school of science and engineering, Professor (10025455)
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| Project Period (FY) |
2004 – 2007
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| Project Status |
Completed (Fiscal Year 2007)
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| Budget Amount *help |
¥3,650,000 (Direct Cost: ¥3,500,000、Indirect Cost: ¥150,000)
Fiscal Year 2007: ¥650,000 (Direct Cost: ¥500,000、Indirect Cost: ¥150,000)
Fiscal Year 2006: ¥800,000 (Direct Cost: ¥800,000)
Fiscal Year 2005: ¥900,000 (Direct Cost: ¥900,000)
Fiscal Year 2004: ¥1,300,000 (Direct Cost: ¥1,300,000)
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| Keywords | protoplanet / SPH / Giant Impacts / planetary accumulation / polytrope / 惑星集積過程 / 月の起源 / 原子惑星 / SPH流体数値計算 / 重力多体系 |
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| Research Abstract |
Collisions between protoplanets are common events in the later stage of planetary formation process. Protoplanets grew into present planets through these collisional events. So it is necessary to obtain information about redistribution of mass and angular momentum between colliding two bodies in order to study the growth rates of planets and the origin of their spin. We have started a series of systematic studies on this theme and this is our first report. We concentrate on the impact between one proto planet, which has one Earth mass, and another protoplanet with 0.06 Earth mass. The motion of two bodies are pursued numerically by the SPH simulation method. We change the minimum distance between the two bodies as parameter to specify the orbital angular momentum of them. For each value of the parameter, we repeated the numerical simulations and obtain final states of bodies. Such various final states are examined by criteria developed to distinguish some clusters formed by many SPH particles. We determine instantaneous orbital elements for relative motion between central protoplanet and each cluster. From this information we forecast the destiny of each cluster, for examples to be merged into the target body or trapped. Then we determine initial conditions result to final characteristic states. The 5 states are merging state in which the impactor absorbed to the target, multiple impact state in which the impactor collide with the target again and again, disruption escaping state in which the impactor is tidally disrupted and a large part of the impactor escapes from the target, trapping state in which the impactor is trapped by the target, and passing state in which the impactor passes through as it is.
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Report
(5 results)
Research Products
(14 results)
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[Presentation] 原始惑星の軌道不安定性2007
Author(s)
榎森 啓元
Organizer
地球惑星科学関連合同大会
Place of Presentation
幕張メッセ国際会議場
Year and Date
2007-05-22
Description
「研究成果報告書概要(和文)」より
Related Report
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