Vertical Structure of a Magnetic Accretion Disk

概要

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The vertical equation of a magnetic disk is solved on the approximation that the disk is geometrically thin, and its whole structure is investigated. The solutions are obtained in the form that we can apply them not only to an accretion flow, but also to a stellar wind. The disk is determined by the values of a thickness parameter of the disk δ (≪1) and the ratio ξ (> 1) of the corotation radius r_c to the Alfven one r_a. It is found that the magnetic disk consisting of a perfectly conductive plasma can exist in the super-Alfvenic region given by 1+δ^3/(2ξ-1)^< 5/2> < r/r_a < ξ^3/δ^< 2/3> For a small ξ(〜0(1)), there occur the sudden concentration of stream lines and a large density gradient in the super-Alfvenic region (r> r_a), even if δ≪1. Therefore, it is necessary that the corotation radius is much larger than the Alfven one (ξ≫1) in order to obtain stable magnetic disks in the super-Alfvenic region.
理論物理学刊行会の論文
1982-08-25