| Project/Area Number |
18K03710
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Multi-year Fund |
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| Section | 一般 |
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| Review Section |
Basic Section 16010:Astronomy-related
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| Research Institution | University of Tsukuba |
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Principal Investigator |
Ohsuga Ken 筑波大学, 計算科学研究センター, 教授 (90386508)
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| Project Period (FY) |
2018-04-01 – 2022-03-31
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| Project Status |
Completed (Fiscal Year 2021)
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| Budget Amount *help |
¥3,770,000 (Direct Cost: ¥2,900,000、Indirect Cost: ¥870,000)
Fiscal Year 2020: ¥1,170,000 (Direct Cost: ¥900,000、Indirect Cost: ¥270,000)
Fiscal Year 2019: ¥1,170,000 (Direct Cost: ¥900,000、Indirect Cost: ¥270,000)
Fiscal Year 2018: ¥1,430,000 (Direct Cost: ¥1,100,000、Indirect Cost: ¥330,000)
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| Keywords | ブラックホール / 中性子星 / 宇宙ジェット / 降着円盤 / 数値シミュレーション / 輻射輸送 / 輻射輸送計算 |
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| Outline of Final Research Achievements |
We performed radiation hydrodynamics/radiation magnetohydrodynamics simulations and radiation transfer calculations to elucidate the origin of ultra-luminous X-ray sources (ULX). As a result, we found two types of outflows are generated from the super-Eddington black hole accretion flows. We then demonstrated that the super-Eddington accretion flow model around a stellar-mass black hole can explain the X-ray luminosity and outflow power of the ULXs. We also revealed the structure and luminosity of the super-Eddington accretion column formed near the magnetic poles of magnetized neutron stars and calculated the shape of the X-ray pulses induced by the rotation of neutron stars. As a result, we showed that the pulsed ULXs can be explained by super-Eddington accretion on magnetized neutron stars.
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| Academic Significance and Societal Importance of the Research Achievements |
本研究では、大規模な輻射流体・輻射磁気流体力学シミュレーションを駆使し、第一原理からブラックホールや中性子星周囲のガス降着およびガス噴出現象、高エネルギー放射の生成機構を解明することに成功した。ブラックホールや中性子星が引き起こす高エネルギー現象は、超強重力場中で物質の運動や光と物質の相互作用によって引き起こされており、それを解き明かした本研究は、高エネルギー天体物理学の解明に加え、相対論等の基礎物理学の解明においても大きく貢献した。
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