Magnetohydrodynamical Accretion Flows : Formation of Magnetic Tower Jet and Subsequent Quasi-Steady State(Poster)
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概要
- 論文の詳細を見る
We present three-dimensional (3-D) magnetohydrodynamical (MHD) simulations of both radiatively inefficient accretion flow (RIAF) into and jet from black holes (BHs). When the bulk of torus material reaches the innermost region close to a central BH, a magnetically driven jet emerges. This magnetic jet is derived by vertically inflating toroidal fields ('magnetic tower') and has a two-component structure : low-β( < 1) plasmas threaded with poloidal fields are surrounded by that with toroidal fields. The collimation width of the jet depends on external pressure, pressure of ambient medium ; the weaker the external pressure is, the wider and the longer-lasting becomes the jet. Unless the external pressure is negligible, the bipolar jet phase ceases after several dynamical timescales at the original torus position and a subsequent quasi-steady state starts.
- 理論物理学刊行会の論文
- 2004-11-15
著者
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KATO Yoshiaki
JAXA/Institute of Space and Astronautical Science
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Mineshige Shin
Yukawa Institute For Theoretical Physics Kyoto University
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KATO Yoshiaki
Yukawa Institute for Theoretical Physics, Kyoto University
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SHIBATA Kazunari
Kwasan and Hida Observatories, Department of Astronomy, Kyoto University
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Shibata Kazunari
Kwasan And Hida Observatories Kyoto University
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Shibata Kazunari
Kwasan And Hida Observatories Department Of Astronomy Kyoto University
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