| Item type |
会議発表論文 / Conference Paper(1) |
| 公開日 |
2015-03-26 |
| タイトル |
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|
タイトル |
Three-dimensional magneto-hydrodynamic simulations of the formation of the inner torus in black hole accretion flows: Brief Instructions for Users of the 'WORKSHOP' Style File |
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言語 |
en |
| 言語 |
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|
言語 |
eng |
| キーワード |
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言語 |
en |
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主題Scheme |
Other |
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主題 |
Accretion disks - MHD - QPOs |
| 資源タイプ |
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資源タイプ識別子 |
http://purl.org/coar/resource_type/c_5794 |
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資源タイプ |
conference paper |
| 著者 |
町田, 真美
松元, 亮治
Machida, Mami
Matsumoto, Ryoji
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| 著者所属 |
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名古屋大学大学院理学研究科天体物理学研究室 |
| 著者所属 |
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千葉大学理学研究科物理学コース |
| 著者所属（英） |
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en |
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Department of Physics and Astrophysics, Nagoya University |
| 著者所属（英） |
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en |
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Department of Physics, Chiba University |
| 出版者 |
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出版者 |
宇宙航空研究開発機構 |
| 出版者（英） |
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出版者 |
Japan Aerospace Exploration Agency (JAXA) |
| 書誌情報 |
宇宙航空研究開発機構特別資料:
en : JAXA Special Publication: The Energetic Cosmos; from Suzaku to ASTRO-H
巻 JAXA-SP-09-008E,
p. 308-309,
発行日 2010-02-26
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| 会議概要（会議名, 開催地, 会期, 主催者等）（英） |
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内容記述タイプ |
Other |
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内容記述 |
The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan |
| 抄録（英） |
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内容記述タイプ |
Other |
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内容記述 |
We present the results of formation of the inner torus in black hole accretion flows obtained from three dimensional magneto-hydrodynamic simulations. We focus on the dependence of numerical results on the gas temperature supplied from the outer region. General relativisitc effects are taken into account using the pseudo-Newtonian potential. We ignore the radiative cooling of the accreting gas. The initial state is a torus threaded by a weak azimuthal magnetic field. We found that mass accretion rate and the mass outflow rate strongly depend on the temperature of the initial torus. In the cool model, a constant angular momentum inner torus is formed around 4-8gamm(sub s) where gamm(sub s) is the Schwarzschild radius. This radius is near the maximum radius of the radial epyciclic frequency. This inner torus deforms itself from a circle to a crescent quasi-periodically. During this deformation, the mass accretion torus returns to a circular shape and starts the next cycle. The time interval of this deformation is caused by the magnetic dynamo activitis driven by MRI. When the magnetic energy released, magnetic pressure driven outflows blow from the inner torus. Power spectral density (PSD) of the time variation of the mass accretion rate in the coolo model has a low frequency peak around 10Hz when we assumed a 10 solar mass black hole. The PSD of the hot model is flat in 1-30Hz. The slope of the PSD in the cool model is steeper than than in the hot model in 30-100Hz. |
| 内容記述（英） |
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内容記述タイプ |
Other |
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内容記述 |
Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science |
| ISSN |
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収録物識別子タイプ |
ISSN |
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収録物識別子 |
1349-113X |
| 書誌レコードID |
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収録物識別子タイプ |
NCID |
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収録物識別子 |
AA11984031 |
| 資料番号 |
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内容記述タイプ |
Other |
|
内容記述 |
資料番号: AA0064574117 |
| レポート番号 |
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内容記述タイプ |
Other |
|
内容記述 |
レポート番号: JAXA-SP-09-008E |
64574117.pdf (1.4 MB)
