| Project/Area Number |
15540230
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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 | The University of Tokyo |
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Principal Investigator |
MAKINO Junichiro The University of Tokyo, Graduate School of Science, Associate Professor, 大学院・理学系研究科, 助教授 (50229340)
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| Co-Investigator(Kenkyū-buntansha) |
FUNATO Yoko The University of Tokyo, Graduate School of Arts and Sciences, Assistant Professor, 大学院・総合文化研究科, 助手 (80292720)
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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 |
¥3,500,000 (Direct Cost: ¥3,500,000)
Fiscal Year 2005: ¥900,000 (Direct Cost: ¥900,000)
Fiscal Year 2004: ¥1,400,000 (Direct Cost: ¥1,400,000)
Fiscal Year 2003: ¥1,200,000 (Direct Cost: ¥1,200,000)
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| Keywords | Parallel algorithms / Special-purpose computers / Stellar Dynamic / Merging instability / Black hole / Dynamical Friction / 並列計算機 / 低レイテンシ通信 / 高密度恒星系 / 球状星団 / 銀河中心 |
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| Research Abstract |
The purpose of this study is to clarify the dynamical evolution of dense stellar systems, such as globular clusters, so-called young and compact clusters, and galactic nuclei, by means of direct N-body simulations. The focus of the study is how the massive black holes grow at the center of these systems. Specifically, we placed two goals. (a) To determine the criterion for the occurrence of the merging instability, in which massive stars merge with other massive stars progressively to form supermassive stars, and (b) to identify the observable signature of massive central black holes in globular clusters and other massive star clusters. As for the condition for the merging instability, we found that the condition is that the initial dynamical friction timescale of massive stars is short (less than 3Mys) and that the initial core radius is fairly small. When fitted by a King mode, W0 must be 8 or larger. For the observational signature of the central black hole, previous observational studies looked for a cusp with slope -7/4, predicted from simple single-component model. By means of N-body calculation in which stellar evolution and stellar mass function are taken into account, we found that the central region of a globular cluster with central massive black hole appears as almost flat core.
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