Formation of Intermediate Mass Black Holes in Star Burst Galaxies
| Project/Area Number |
14540225
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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 | Nagoya University |
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Principal Investigator |
IKEUCHI Satoru Nagoya University, Graduate School of Science, Physics Department, Professor, 大学院・理学研究科, 教授 (90025461)
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| Project Period (FY) |
2002 – 2004
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| Project Status |
Completed (Fiscal Year 2004)
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| Budget Amount *help |
¥3,600,000 (Direct Cost: ¥3,600,000)
Fiscal Year 2004: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 2003: ¥1,400,000 (Direct Cost: ¥1,400,000)
Fiscal Year 2002: ¥1,600,000 (Direct Cost: ¥1,600,000)
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| Keywords | Intermediate Mass Black Holes / Super Massive Black Hole / Stellar Remnant / Coee-Halo Structure / Star Burst / Galaxy M82 / Three-Body Collision / Distant Two-Body Encounter / 高密度星団系 / M82 / ガスの粘性抵抗 / 大質量ブラックホール / 激しい緩和過程 / ブラックホール / 巨大銀河風 / 高光度X線源 / チムニー構造 / 分子雲 / 活動的銀河核 / 電波輝線 |
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| Research Abstract |
As the three points of this research are set in the followings : (1)Star burst phenomena in high dense stellar systems, (2)Formation of intermediate mass black holes(IMBH)s due to the gravitational interaction of Stellar remnants, and (3)Growth to super massive black holes(SMBHs) due to gravitational interaction of IMBHs. These three steps can be divided to each independent process.
At first in the step (1), it is examined what remnants are formed in a star burst phenomenon. Since stellar black holes and neutron stars are too few to form an IMBH for a usual mass function, it is shown that a flatter mass function must be considered. In the following step (2), if we assume the distribution of stellar remnants to be the same as stellar distribution and velocity distribution to be usual Gaussian distribution, the stellar remnant system evolved to the core-halo structure due to distant two-body gravitational interaction. Soon, the three-body collisions become effective and remnant system evo
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lved to high dense system. The difficult problem is that the contraction of remnant system becomes so slow because of adiabatic contraction that the IMBH can not be formed within 10 Gy. Then, assuming the co-existence of gas-component, we included the gas drag effects and the shock dissipation due to supersonic motions. However, the cooling effect is too small to affect the evolution. The resultant remnant system is the radius 10pc and mass 100,000 solar mass. This size is too large for the formation of IMBH. As for the step (3), we examined the conditions for the formation of an SMBH within 10 Gy. It is concluded that the IMBHs must be accumulated with size 1pc and mass 1 million solar mass. If so, the difference between the size of high density remnant system formed in (2)and the necessitated size for the formation of SMBH is 4 digits, this gap is very difficult to coincide. Therefore, in the step from (2)to (3), we must include some new physical processes which are not considered in this work. This problem is the subjects of future research. Less
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Report
(4 results)
Research Products
(9 results)
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[Book] 寺田寅彦と現代2005
Author(s)
池内 了
Publisher
みすず書房
Description
「研究成果報告書概要(和文)」より
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