General Structure of Steady Accretion Disks with a Magnetic Field
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概要
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By using the magneto-hydrodynamic equations, we analyze the basic equations describing magnetic accretion disks on the two characteristic surfaces; (a) the Alfven surface where the accretion velocity is equal to the Alfven one and (b) the boundary surface where the matter density becomes zero. It is found that the accretion flow always has the super-Alfvenic velocity on the boundary surface, while it can pass from the super-Alfvenic region to the sub-Alfvenic one near the equatorial plane. The transfer of angular momentum by magnetic tension takes place enormously near the Alfven surface on the boundary, and the Alfven radius should be much larger than the Keplerian radius in order to obtain stable accretion disks.
- 理論物理学刊行会の論文
- 1979-08-25
著者
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冨松 彰
名古屋大 理
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TOMIMATSU Akira
Research Institute for Theoretical Physics Hiroshima University
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Horiuchi Ritoku
Research Institute For Theoretical Physics Hiroshima University
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Tomimatsu Akira
Research Institute For Technical Physics Hiroshima University
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